What is Binding Energy?

The atomic structure. Credit: Encyclopædia Britannica, Inc.

Have you ever taken a look at a piece of firewood and said to yourself, “gee, I wonder how much energy it would take to split that thing apart”? Chances are, no you haven’t, few people do. But for physicists, asking how much energy is needed to separate something into its component pieces is actually a pretty important question.

In the field of physics, this is what is known as binding energy, or the amount of mechanical energy it would take to disassemble an atom into its separate parts. This concept is used by scientists on many different levels, which includes the atomic level, the nuclear level, and in astrophysics and chemistry.

Nuclear Force:

As anyone who remembers their basic chemistry or physics surely knows, atoms are composed of subatomic particles known as nucleons. These consist of positively-charged particles (protons) and neutral particles (neutrons) that are arranged in the center (in the nucleus). These are surrounded by electrons which orbit the nucleus and are arranged in different energy levels.

Neils Bohr's model a nitrogen atom. Credit: britannica.com
Neils Bohr’s model a nitrogen atom. Credit: britannica.com

The reason why subatomic particles that have fundamentally different charges are able to exist so close together is because of the presence of Strong Nuclear Force – a fundamental force of the universe that allows subatomic particles to be attracted at short distances. It is this force that counteracts the repulsive force (known as the Coulomb Force) that causes particles to repel each other.

Therefore, any attempt to divide the nucleus into the same number of free unbound neutrons and protons – so that they are far/distant enough from each other that the strong nuclear force can no longer cause the particles to interact – will require enough energy to break these nuclear bonds.

Thus, binding energy is not only the amount of energy required to break strong nuclear force bonds, it is also a measure of the strength of the bonds holding the nucleons together.

Nuclear Fission and Fusion:

In order to separate nucleons, energy must be supplied to the nucleus, which is usually accomplished by bombarding the nucleus with high energy particles. In the case of bombarding heavy atomic nuclei (like uranium or plutonium atoms) with protons, this is known as nuclear fission.

Nuclear fission, where an atom of Uranium 96 is split by a free neutron to produce barium and krypton. Credit: physics.stackexchange.com
Nuclear fission, where an atom of Uranium 96 is split by a free neutron to produce barium and krypton. Credit: physics.stackexchange.com

However, binding energy also plays a role in nuclear fusion, where light nuclei together (such as hydrogen atoms), are bound together under high energy states. If the binding energy for the products is higher when light nuclei fuse, or when heavy nuclei split, either of these processes will result in a release of the “extra” binding energy. This energy is referred to as nuclear energy, or loosely as nuclear power.

It is observed that the mass of any nucleus is always less than the sum of the masses of the individual constituent nucleons which make it up. The “loss” of mass which results when nucleons are split to form smaller nucleus, or merge to form a larger nucleus, is also attributed to a binding energy. This missing mass may be lost during the process in the form of heat or light.

Once the system cools to normal temperatures and returns to ground states in terms of energy levels, there is less mass remaining in the system. In that case, the removed heat represents exactly the mass “deficit”, and the heat itself retains the mass which was lost (from the point of view of the initial system). This mass appears in any other system which absorbs the heat and gains thermal energy.

Types of Binding Energy:

Strictly speaking, there are several different types of binding energy, which is based on the particular field of study. When it comes to particle physics, binding energy refers to the energy an atom derives from electromagnetic interaction, and is also the amount of energy required to disassemble an atom into free nucleons.

Nuclear Physics
Diagram showing the process of nuclear fusion. Credit: Lancaster University

In the case of removing electrons from an atom, a molecule, or an ion, the energy required is known as “electron binding energy” (aka. ionization potential). In general, the binding energy of a single proton or neutron in a nucleus is approximately a million times greater than the binding energy of a single electron in an atom.

In astrophysics, scientists employ the term “gravitational binding energy” to refer to the amount of energy it would take to pull apart (to infinity) an object held together by gravity alone – i.e. any stellar object like a star, a planet, or a comet. It also refers to the amount of energy that is liberated (usually in the form of heat) during the accretion of such an object from material falling from infinity.

Finally, there is what is known as “bond” energy, which is a measure of the bond strength in chemical bonds, and is also the amount of energy (heat) it would take to break a chemical compound down into its constituent atoms. Basically, binding energy is the very thing that binds our Universe together. And when various parts of it are broken apart, it is the amount of energy needed to carry it out.

The study of binding energy has numerous applications, not the least of which are nuclear power, electricity, and chemical manufacture. And in the coming years and decades, it will be intrinsic in the development of nuclear fusion!

We have written many articles about binding energy for Universe Today. Here’s What is Bohr’s Atomic Model?, What is John Dalton’s Atomic Model?, What is the Plum Pudding Atomic Model?, What is Atomic Mass?, and Nuclear Fusion in Stars.

If you’d like more info on binding energy, check out Hyperphysics article on Nuclear Binding Energy.

We’ve also recorded an entire episode of Astronomy Cast all about the Important Numbers in the Universe. Listen here, Episode 45: The Important Numbers in the Universe.

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Antares Return to Flight Set for Magnificent Monday Night Launch – Watch Live

The Orbital ATK Antares rocket, with the Cygnus OA-5 spacecraft onboard, is raised into the vertical position on launch Pad-0A for planned launch on Oct. 17, 2016, at NASA's Wallops Flight Facility in Virginia. Credit: Ken Kremer/kenkremer
The Orbital ATK Antares rocket, with the Cygnus OA-5 spacecraft onboard, is raised into the vertical position on launch Pad-0A for planned launch on Oct. 17, 2016, at NASA's Wallops Flight Facility in Virginia. Credit: Ken Kremer/kenkremer
The Orbital ATK Antares rocket, with the Cygnus OA-5 spacecraft onboard, is raised into the vertical position on launch Pad-0A for planned launch on Oct. 17, 2016, at NASA’s Wallops Flight Facility in Virginia. Credit: Ken Kremer/kenkremer

NASA WALLOPS FLIGHT FACILITY, VA – The ‘Return to Flight’ blastoff of Orbital ATK’s upgraded Antares rocket will have to wait one more day to come to fruition with a magnificent Monday night launch – after a technical scrub was called this afternoon, Oct. 16, at NASA’s Virginia launch base due to a faulty cable.

The launch potentially offers a thrilling skyshow to millions of US East Coast spectators if all goes well.

Antares Launch Viewing Map. This “first-sight” map indicates potential to see Orbital ATK’s Antares rocket in the minutes following its launch on the OA-5 mission to the ISS on October 16, 2016. Credit: Orbital ATK
Antares Launch Viewing Map. This “first-sight” map indicates potential to see Orbital ATK’s Antares rocket in the minutes following its launch on the OA-5 mission to the ISS on October 16, 2016. Credit: Orbital ATK

Despite picture perfect Fall weather, technical gremlins intervened to halt Sunday nights planned commercial cargo mission for NASA carrying 2.5 tons of science and supplies bound for the International Space Station (ISS).

The launch of the Orbital ATK CRS-5 mission is now scheduled for October 17 at 7:40 p.m. EDT, from the Mid-Atlantic Regional Spaceport pad 0A at NASA’s Wallops Flight Facility on Virginia’s picturesque Eastern shore.

You can watch the launch live on NASA TV as well as the agency’s website beginning at 6:30 p.m. EDT Oct 17.

Mondays liftoff is slated to take place approximately 23 minutes earlier then Sunday’s hoped for time of 8:03 p.m. EDT in order to match the moment when the orbital plane of the station passes on NASA Wallops.

The weather outlook on Monday remains extremely favorable with a 95 percent chance of acceptable conditions at launch time.

A nearly full moon has risen over Antares the past few days at the launch pad.

2 Moons and Antares on the launch pad on the evening of Oct. 15, 2016 at NASA's Wallops Flight Facility in Virginia in this water reflection shot.  Liftoff of the OA-5 mission to the ISS is planned for Oct. 17, 2016. Credit: Ken Kremer/kenkremer
2 Moons and Antares on the launch pad on the evening of Oct. 15, 2016 at NASA’s Wallops Flight Facility in Virginia in this water reflection shot. Liftoff of the OA-5 mission to the ISS is planned for Oct. 17, 2016. Credit: Ken Kremer/kenkremer

Announcement of the launch scrub of the mission – also known as OA-5 – came just as the six hour countdown was set to begin after engineers discovered the bad cable.

“Today’s launch of Orbital ATK’s Antares rocket is postponed 24 hours due to a ground support equipment (GSE) cable that did not perform as expected during the pre-launch check out,” officials at NASA Wallops said.

The faulty cable was a component of the rocket’s hold down system at the pad, Orbital ATK officials told Universe Today after the scrub was announced.

Technicians have spares on hand and are working now to replace the cable in time to permit a Monday evening launch.

“We have spares on hand and rework procedures are in process. The Antares and Cygnus teams are not currently working any technical issues with the rocket or the spacecraft.”

Besides the cable the rocket is apparently in perfect shape.

“The Antares and Cygnus teams are not currently working any technical issues with the rocket or the spacecraft.”

Antares launches have been on hold for two years after it was grounded following its catastrophic failure just moments after liftoff on Oct. 28, 2014 that doomed the Orb-3 resupply mission to the space station – as witnessed by this author.

Orbital ATK’s Antares commercial rocket had to be overhauled with the completely new RD-181 first stage engines- fueled by LOX/kerosene – following the destruction of the Antares rocket and Cygnus supply ship two years ago.

The 14 story tall commercial Antares rocket also will launch for the first time in the upgraded 230 configuration – powered by new Russian-built first stage engines designed and manufactured by Energomesh.

The 133-foot-tall (40-meter) Antares was rolled out to pad 0A on Thursday, Oct. 13 – three days prior to Sunday’s intended launch date. It was raised to the vertical launch position on Friday.

The Orbital ATK Antares rocket, with the Cygnus OA-5 spacecraft onboard, is raised into the vertical position on launch Pad-0A for planned launch on Oct. 17, 2016, at NASA's Wallops Flight Facility in Virginia. Credit: Ken Kremer/kenkremer
The Orbital ATK Antares rocket, with the Cygnus OA-5 spacecraft onboard, is raised into the vertical position on launch Pad-0A for planned launch on Oct. 17, 2016, at NASA’s Wallops Flight Facility in Virginia. Credit: Ken Kremer/kenkremer

The two stage Antares will carry the Orbital OA-5 Cygnus cargo freighter to orbit on a flight bound for the ISS and its multinational crew of astronauts and cosmonauts.

The launch marks the first nighttime liftoff of the Antares – and it could be visible up and down the eastern seaboard if weather and atmospheric conditions cooperate to provide a spectacular viewing opportunity to the most populated region in North America.

The Cygnus spacecraft for the OA-5 mission is named the S.S. Alan G. Poindexter in honor of former astronaut and Naval Aviator Captain Alan Poindexter.

Under the Commercial Resupply Services (CRS) contract with NASA, Orbital ATK will deliver approximately 28,700 kilograms of cargo to the space station. OA-5 is the sixth of these missions.

Antares and the Moon at the pad at NASA's Wallops Flight Facility in Virginia as seen from a boat off shore in the Atlantic Ocean on Oct. 15, 2016. Credit: © Patrick J. Hendrickson / Highcamera.com
Antares and the Moon at the pad at NASA’s Wallops Flight Facility in Virginia as seen from a boat off shore in the Atlantic Ocean on Oct. 15, 2016. Credit: © Patrick J. Hendrickson / Highcamera.com

Watch for Ken’s continuing Antares/Cygnus mission and launch reporting. He will be reporting from on site at NASA’s Wallops Flight Facility, VA during the launch campaign.

Stay tuned here for Ken’s continuing Earth and Planetary science and human spaceflight news.

Ken Kremer

What are Volcanoes?

Image taken by a crew member of Expedition 13 from the ISS, showing the eruption of Cleveland Volcano, Aleutian Islands, Alaska. Credit: NASA

A volcano is an impressive sight. When they are dormant, they loom large over everything on the landscape. When they are active, they are a destructive force of nature that is without equal, raining fire and ash down on everything in site. And during the long periods when they are not erupting, they can also be rather beneficial to the surrounding environment.

But just what causes volcanoes? When it comes to our planet, they are the result of active geological forces that have shaped the surface of the Earth over the course of billions of years. And interestingly enough, there are plenty of examples of volcanoes on other bodies within our Solar System as well, some of which put those on Earth to shame!

Definition:

By definition, a volcano is a rupture in the Earth’s (or another celestial body’s) crust that allows hot lava, volcanic ash, and gases to escape from a magma chamber located beneath the surface. The term is derived from Vulcano, a volcanically-active island located of the coast of Italy who’s name in turn comes from the Roman god of fire (Vulcan).

The Earth's Tectonic Plates. Credit: msnucleus.org
Artist’s illustration of the Earth’s Tectonic Plates. Credit: msnucleus.org

On Earth, volcanoes are the result of the action between the major tectonic plates. These sections of the Earth’s crust are rigid, but sit atop the relatively viscous upper mantle. The hot molten rock, known as magma, is forced up to the surface – where it becomes lava. In short, volcanoes are found where tectonic plates are diverging or converging – such as the Mid-Atlantic Ridge or the Pacific Ring of Fire – which causes magma to be forced to the surface.

Volcanoes can also form where there is stretching and thinning of the crust’s interior plates, such as in the the East African Rift and the Rio Grande Rift in North America. Volcanism can also occur away from plate boundaries, where upwelling magma is forced up into brittle sections of the crust, forming volcanic islands – such as the Hawaiian islands.

Erupting volcanoes pose many hazards, and not just to the surrounding countryside. In their immediate vicinity, hot, flowing lava can cause extensive damage to the environment, property, and endanger lives. However, volcanic ash can cause far-reaching damage, raining sulfuric acid, disrupting air travel, and even causing “volcanic winters” by obscuring the Sun (thus triggering local crop failures and famines).

Types of Volcanoes:

There are four major types of volcanoes – cinder cone, composite and shield volcanoes, and lava domes. Cinder cones are the simplest kind of volcano, which occur when magma is ejected from a volcanic vent. The ejected lava rains down around the fissure, forming an oval-shaped cone with a bowl-shaped crater on top. They are typically small, with few ever growing larger than about 300 meters (1,000 feet) above their surroundings.

Cinder cone Paricutin. Image credit: USGS
Paricutin, an example of a cinder cone volcano. Credit: USGS

Composite volcanoes (aka. stratovolcanoes) are formed when a volcano conduit connects a subsurface magma reservoir to the Earth’s surface. These volcanoes typically have several vents that cause magma to break through the walls and spew from fissures on the sides of the mountain as well as the summit.

These volcanoes are known for causing violent eruptions. And thanks to all this ejected material, these volcanoes can grow up to thousands of meters tall. Examples include Mount Rainier (4,392 m; 14,411 ft), Mount Fuji (3,776 m; 12,389 ft), Mount Cotopaxi (5,897 m; 19,347 ft) and Mount Saint Helens (2,549 mm; 8,363 ft).

Shield volcanoes are so-named because of their large, broad surfaces. With these types of volcanoes, the lava that pours forth is thin, allowing it to travel great distances down the shallow slopes. This lava cools and builds up slowly over time, with hundreds of eruptions creating many layers. They are therefore not likely to be catastrophic. Some of the best known examples are those that make up the Hawaiian Islands, especially Mauna Loa and Mauna Kea.

Volcanic or lava domes are created by small masses of lava which are too viscous to flow very far. Unlike shield volcanoes, which have low-viscosity lava, the slow-moving lava simply piles up over the vent. The dome grows by expansion over time, and the mountain forms from material spilling off the sides of the growing dome. Lava domes can explode violently, releasing a huge amount of hot rock and ash.

Artist's impression of a what lies beneath the Yellowstone volcano. Credit: Hernán Cañellas/National Geographic
Artist’s impression of a what lies beneath the Yellowstone volcano. Credit: Hernán Cañellas/National Geographic

Volcanoes can also be found on the ocean floor, known as submarine volcanoes. These are often revealed through the presence of blasting steam and rocky debris above the ocean’s surface, though the pressure of the ocean’s water can often prevent an explosive release.

In these cases, lava cools quickly on contact with ocean water, and forms pillow-shaped masses on the ocean floor (called pillow lava). Hydrothermal vents are also common around submarine volcano, which can support active and peculiar ecosystems because of the energy, gases and minerals they release. Over time, the formations created by submarine volcanoes may become so large that they become islands.

Volcanoes can also developed under icecaps, which are known as subglacial volcanoes. In these cases, flat lava flows on top of pillow lava, which results from lava quickly cooling upon contact with ice. When the icecap melts, the lava on top collapses, leaving a flat-topped mountain. Very good examples of this type of volcano can be seen in Iceland and British Columbia, Canada.

Examples on Other Planets:

Volcanoes can be found on many bodies within the Solar System. Examples include Jupiter’s moon Io, which periodically experiences volcanic eruptions that reach up to 500 km (300 mi) into space. This volcanic activity is caused by friction or tidal dissipation produced in Io’s interior, which is responsible for melting a significant amount of Io’s mantle and core.

Model of the possible interior composition of Io with various features labelled. Credit: Wikipedia Commons/Kelvinsong
Model of the possible interior composition of Io with various features labelled. Credit: Wikipedia Commons/Kelvinsong

It’s colorful surface (orange, yellow, green, white/grey, etc.) shows the presence of sulfuric and silicate compounds, which were clearly deposited by volcanic eruptions. The lack of impact craters on its surface, which is uncommon on a Jovian moon, is also indicative of surface renewal.

Mars has also experienced intense volcanic activity in its past, as evidenced by Olympus Mons – the largest volcano in the Solar System. While most of its volcanic mountains are extinct and collapsed, the Mars Express spacecraft observed evidence of more recent volcanic activity, suggesting that Mars may still be geologically active.

Much of Venus’ surface has been shaped by volcanic activity as well. While Venus has several times the number of Earth’s volcanoes, they were believed to all be extinct. However, there is a multitude of evidence that suggests that there may still be active volcanoes on Venus which contribute to its dense atmosphere and runaway Greenhouse Effect.

For instance, during the 1970s, multiple Soviet Venera missions conducted surveys of Venus. These missions obtained evidence of thunder and lightning within the atmosphere, which may have been the result of volcanic ash interacting with the atmosphere. Similar evidence was gathered by the ESA’s Venus Express probe in 2007.

3-D perspective of the Venusian volcano, Maat Mons generated from radar data from NASA’s Magellan mission.
3-D perspective of the Venusian volcano, Maat Mons generated from radar data from NASA’s Magellan mission. Credit: NASA/JPL

This same mission observed transient localized infrared hot spots on the surface of Venus in 2008 and 2009, specifically in the rift zone Ganis Chasma – near the shield volcano Maat Mons. The Magellan probe also noted evidence of volcanic activity from this mountain during its mission in the early 1990s, using radar-sounding to detect ash flows near the summit.

Cryovolcanism:

In addition to “hot volcanoes” that spew molten rock, there are also cryovolcanoes (aka. “cold volcanoes”). These types of volcanoes involve volatile compounds  – i.e. water, methane and ammonia – instead of lava breaking through the surface. They have been observed on icy bodies in the Solar System where liquid erupts from ocean’s hidden in the moon’s interior.

For instance, Jupiter’s moon Europa, which is known to have an interior ocean, is believed to experiences cryovolcanism. The earliest evidence for this had to do with its smooth and young surface, which points towards endogenic resurfacing and renewal. Much like hot magma, water and volatiles erupt onto the surface where they then freeze to cover up impact craters and other features.

In addition, plumes of water were observed in 2012 and again in 2016 using the Hubble Space Telescope. These intermittent plumes were observed on both occasions to be coming in the southern region of Europa, and were estimated to be reach up to 200 km (125 miles) before depositing water ice and material back onto the surface.

In 2005, the Cassini-Huygens mission detected evidence of cryovolcanism on Saturn’s moons Titan and Enceladus. In the former case, the probe used infrared imaging to penetrate Titan’s dense clouds and detect signs of a 30 km (18.64 mi) formation, which was believed to be caused by the upwelling of hydrocarbon ices beneath the surface.

On Enceladus, cryovolcanic activity has been confirmed by observing plumes of water and organic molecules being ejected from the moon’s south pole. These plumes are are thought to have originated from the moon’s interior ocean, and are composed mostly of water vapor, molecular nitrogen, and volatiles (such as methane, carbon dioxide and other hydrocarbons).

In 1989, the Voyager 2 spacecraft observed cryovolcanoes ejecting plumes of water ammonia and nitrogen gas on Neptune’s moon Triton. These nitrogen geysers were observed sending plumes of liquid nitrogen 8 km (5 mi) above the surface of the moon. The surface is also quite young, which was seen as indication of endogenic resurfacing. It is also theorized that cryovolcanism may also be present on the Kuiper Belt Object Quaoar.

Here on Earth, volcanism takes the form of hot magma being pushed up through the Earth’s silicate crust due to convention in the interior. However, this kind of activity is present on all planet that formed from silicate material and minerals, and where geological activity or tidal stresses are known to exist. But on other bodies, it consists of cold water and materials from the interior ocean being forced through to the icy surface.

Color Mosaic of Olympus Mons on Mars
Color Mosaic of Olympus Mons on Mars. Credit: NASA/JPL

Today, our knowledge of volcanism (and the different forms it can take) is the result of improvements in both the field of geology, as well as space exploration. The more we learn of about other planets, the more we are able to see startling similarities and contrasts with our own (and vice versa).

We have written many interesting articles about volcanoes here at Universe Today. Here’s 10 Interesting Facts About Volcanoes, What are the Different Types of Volcanoes?, How Do Volcanoes Erupt?, What Are The Benefits Of Volcanoes?, What is the Difference Between Active and Dormant Volcanoes?

For more information, be sure to check out What is a Volcano? at NASA Space Place.

Astronomy Cast has an episode on the subject – Episode 141: Volcanoes Hot and Cold.

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What is the Wettest Place on Earth?

Countries by average annual precipitation. Credit: Wikipedia Commons/Atila Kagan

Those who live along the “wet coast” – which is what people living in Puget Sound or the lower mainland of British Columbia and Vancouver Island affectionately call their home – might think that they live in the wettest place on Earth. Then again, people living in the Amazon rain forest might think that there lush and beautiful home is the dampest place in the world.

But in truth, all these places come up dry (pun intended!) compared to the one place that has held the title for wettest point on Earth many times in its history. And that place is none other than Mawsynram, India, which experiences an annual average rainfall of 12 meters. And yet, this curious region in northwestern part of the Indian subcontinent is an exercise in extremes, either drowning in rainwater, or starving for it.

Annual Rainfall:

When it comes to describing locations on planet Earth in terms of “wet”, some clarifications are needed. What we are talking about is average annual precipitation – i.e. rainfall, snow, drizzle, fog, etc. – measured in mm (or inches). This is necessary because otherwise, the “wettest” place on Earth would be the Mariana Trench, which has over 10,000 meters (36,000 feet) of water on top of it.

Cherrapunji, one of the wettest places on Earth. Credit: Public Domain
Cherrapunji, one of the wettest places on Earth. Credit: Public Domain

Also, based on rainfall. the wettest place on Earth has been known to change from time to time. In recent years, that title has gone to the town of Mawsynram, a village located in the East Khasi Hills district of northeastern, India. With an average annual rainfall of 11,872 millimetres (467.4 in), it is arguably the wettest place on Earth.

However, it is often in competition with the neighboring town of Cherrapunjee, which is located just 15 km (9.3 mi) to the west of Mawsynram in the East Khasi Hills district in northeastern India. The city’s yearly rainfall average stands at 11,777 millimetres (463.7 in), so it too has held the title.

The reason for these town experiencing so much precipitation has to do with the local climate. Situated within a subtropical highland climate zone, it experiences a lengthy and powerful monsoon season. In once instance, the monsoon season lasted for 2 years straight with no reported break in the rain!

Surprisingly, the high rainfall is a result of the region’s elevation and not the monsoon season alone. Huge amounts of warm air condense and fall as rain when they encounter the Khasi Hills. The topography of the region forces the very moist clouds up and down, forcing them to empty their accumulated water over the region.

Seven Sisters' falls, located in the East Khasi Hills district. Credit: Wikipedia Commons/Rishav999
Seven Sisters’ falls, located in the East Khasi Hills district. Credit: Wikipedia Commons/Rishav999

Other Locations:

Beyond northeastern India, there are several other locations on the planet that experience over 10 meters (32.8 feet) of annual precipitation. For instance, the town of Tutunendo, Colombia, experiences an average of 11,770 mm (463.38 in) of annual rainfall. The area actually experiences two rainy seasons a year, so precipitation is pretty much the norm.

Next up, there is Mount Waialeale, a shield volcano located on the island of Kaua’i on the Hawaiian Islands. As the the second highest point on the island, its name literally means “rippling water” (or “overflowing water”), and for good reason! This mountain has had an average of 11,500 mm (452 in) of rainfall since 1912.

However, in 1982, its summit experienced 17,300 mm (683 in), making it the wettest place on Earth in that year. And between 1978-2007, Big Bog – a spot in Haleakala National Park on the island of Maui, Hawaii – experienced an average of 10,300 mm (404 in) of rainfall, putting it in the top ten.

Wai?ale?ale (or 'Rippling Waters') Lake
Waialeale (or ‘Rippling Waters’) Lake, located atop Mount Waialeale on the island of Kaua’i, Hawaii. Credit: Wikipedia Commons/Volcantrek8

As already noted, the “wettest place on Earth” changes over time. This should come as no surprise, considering that weather patterns have been known to shift, not only in the course of an average year, but also over the course of centuries and millennia.

Nevertheless, those places that experience over 10 meters of precipitation are generally found within the tropical regions of the world, places known for experiencing intense and prolonged rainy seasons, and where lush tropical rainforests have existed for thousands of years. Here is a recent list of the top 10 locations.

But with anthropogenic climate change becoming a growing factor in planetary weather systems, this too could be subject to change. In the coming decades, and centuries, who’s to say where the most precipitation will fall on planet Earth?

We have written many interesting articles about rainfall and precipitation here at Universe Today. Here’s What are Tornadoes?, What is Tornado Alley?, Where do Hurricanes Occur?, What is a Warm Front?, and How Does Fog Form?

For more information, check out the US Geological Survey’s page on Precipitation: The Water Cycle and NASA’s Global Precipitation Measurement page.

Astronomy Cast also has an episode on the subject – Episode 226: Weather

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The Moon Is Getting Slammed Way More Than We Thought

A brand new crater on the Moon! This new 12 meter (39 foot) diameter impact crater formed between 25 October 2012 and 21 April 2013 Credit: NASA/GSFC/Arizona State University].
Animation of a temporal pair of the new 39-foot (12-meter) impact crater on the moon photographed by NASA's Lunar Reconnaissance Orbiter Credit: NASA/GSFC/Arizona State University
Animation of a temporal pair of the new 39-foot (12-meter) impact crater on the moon photographed by NASA’s Lunar Reconnaissance Orbiter Credit: NASA/GSFC/Arizona State University

We often hear how the Moon’s appearance hasn’t changed in millions or even billions of years. While micrometeorites, cosmic rays and the solar wind slowly grind down lunar rocks, the Moon lacks erosional processes such as water, wind and lurching tectonic plates that can get the job done in a hurry.

After taking the first boot print photo, Aldrin moved closer to the little rock and took this second shot. The dusty, sandy pebbly soil is also known as the lunar ‘regolith’. Click to enlarge. Credit: NASA
One of a series of photos Apollo 11 astronaut Edwin Aldrin made of his bootprint in the dusty, sandy lunar soil, called regolith. Based on a newy study, the impression may disappear in a few tens of thousands of years instead a few million. Credit: NASA

Remember Buzz Aldrin’s photo of his boot print in the lunar regolith? It was thought the impression would last up to 2 million years. Now it seems that estimate may have to be revised based on photos taken by the Lunar Reconnaissance Orbiter (LRO) that reveal that impacts are transforming the surface much faster than previously thought.

Distribution of new impact craters (yellow dots) discovered by analyzing 14,000 NAC temporal pairs. The two red dots mark the location of the 17 March 2013 and the 11 September 2013 impacts that were recorded by Earth-based video monitoring [NASA/GSFC/Arizona State University]
This map shows the distribution of new impact craters (yellow dots) discovered by analyzing 14,000 narrow-angle camera (NAC) temporal pairs. The two red dots mark the location of the March 17, 2013 and September 11, 2013 impacts that were recorded by Earth-based video monitoring. LRO’s mission was recently extended an addition two years through September 2018. Credit: NASA/GSFC/ASU
The LRO’s high resolution camera, which can resolve features down to about 3 feet (1-meter) across, has been peering down at the Moon from orbit since 2009. Taking before and after images, called temporal pairs, scientists have identified 222 impact craters that formed over the past 7 years. The new craters range from 10 feet up to 141 feet (3-43 meters) in diameter.

By analyzing the number of new craters and their size, and the time between each temporal pair, a team of scientists from Arizona State University and Cornell estimated the current cratering rate on the Moon. The result, published in Nature this week, was unexpected: 33% more new craters with diameters of at least 30 feet (10 meters) were found than anticipated by previous cratering models.

their brightest recorded flash occurred on 17 March 2013 with coordinates 20.7135°N, 335.6698°E. Since then LRO passed over the flash site and the NAC imaged the surrounding area; a new 18 meter (59 feet) diameter crater was found by comparing images taken before and after the March date.
LRO before and after images of an impact event on March 17, 2013. The newly formed crater is 59 feet (18 meters) in diameter. Subsurface regolith not exposed to sunlight forms a bright halo around the new crater. There also appears to be a larger nimbus of darker reflectance material visible much further beyond but centered on the impact. Credit: NASA/GSFC/Arizona State University

Similar to the crater that appeared on March 17, 2013 (above), the team also found that new impacts are surrounded by light and dark reflectance patterns related to material ejected during crater formation. Many of the larger impact craters show up to four distinct bright or dark reflectance zones. Nearest to the impact site, there are usually zone of both high and low reflectance.  These two zones likely formed as a layer of material that was ejected from the crater during the impact shot outward to about 2½ crater diameters from the rim.

An artist's illustration of a meteoroid impact on the Moon. (Credit: NASA).
An artist’s illustration of a meteoroid impact on the Moon. Impacts dig up fresh material from below as well as send waves of hot rock vapor and molten rock across the lunar landscape, causing a much faster turnover of the moon soil than previously thought. Credit: NASA

From analyzing multiple impact sites, far flung ejecta patterns wrap around small obstacles like hills and crater rims, indicating the material was traveling nearly parallel to the ground. This kind of path is only possible if the material was ejected at very high speed around 10 miles per second or 36,000 miles per hour! The jet contains vaporized and molten rock that disturb the upper layer of lunar regolith, modifying its reflectance properties.


How LRO creates temporal pairs and scientists use them to discover changes on the moon’s surface.

In addition to discovering impact craters and their fascinating ejecta patterns, the scientists also observed a large number of small surface changes they call ‘splotches’ most likely caused by small, secondary impacts. Dense clusters of these splotches are found around new impact sites suggesting they may be secondary surface changes caused by material thrown out from a nearby primary impact. From 14,000 temporal pairs, the group identified over 47,000 splotches so far.

Example of a low reflectance (top) and high reflectance (bottom) splotch created either by a small impactor or more likely from secondary ejecta. In either case, the top few centimeters of the regolith (soil) was churned [NASA/GSFC/Arizona State University].
Here are two examples of a low reflectance (top) and high reflectance (bottom) splotch created either by a small impactor or more likely from secondary ejecta. In either case, the top few inches of the regolith (soil) was churned Credit: NASA/GSFC/Arizona State University
Based on estimates of size, depth and frequency of formation, the group estimated that the relentless churning caused by meteoroid impacts will turn over 99% of the lunar surface after about 81,000 years. Keep in mind, we’re talking about the upper regolith, not whole craters and mountain ranges. That’s more than 100 times faster than previous models that only took micrometeorites into account. Instead of millions of years for those astronaut boot prints and rover tracks to disappear, it now appears that they’ll be wiped clean in just tens of thousands!

Antares Raised to Launch Position for Sunday Night Launch to ISS

The Orbital ATK Antares rocket, with the Cygnus spacecraft onboard, is raised into the vertical position on launch Pad-0A, Friday, Oct. 14, 2016 at NASA's Wallops Flight Facility in Virginia. Credit: NASA/Bill Ingalls
The Orbital ATK Antares rocket, with the Cygnus spacecraft onboard, is raised into the vertical position on launch Pad-0A, Friday, Oct. 14, 2016 at NASA's Wallops Flight Facility in Virginia.  Credit: NASA/Bill Ingalls
The Orbital ATK Antares rocket, with the Cygnus spacecraft onboard, is raised into the vertical position on launch Pad-0A, Friday, Oct. 14, 2016 at NASA’s Wallops Flight Facility in Virginia. Credit: NASA/Bill Ingalls

NASA WALLOPS FLIGHT FACILITY, VA – After a two year stand down, an upgraded commercial Antares rocket was rolled out to the NASA Wallops launch pad on Virginia’s eastern shore and raised to its launch position today in anticipation of a spectacular Sunday night liftoff, Oct. 16, to the International Space Station (ISS) on a critical resupply mission for NASA.

Blastoff of the re-engined Orbital ATK Antares rocket is slated for 8:03 p.m. EDT on Oct. 16 from the Mid-Atlantic Regional Spaceport pad 0A at NASA’s Wallops Flight Facility on Virginia’s picturesque Eastern shore.

The two year lull in Antares launches followed the rockets immediate grounding after its catastrophic failure just moments after liftoff on Oct. 28, 2014 that doomed the Orb-3 resupply mission to the space station – as witnessed by this author.

Officials had to postpone this commercial resupply mission – dubbed OA-5 – from mid-week due to Cat 3 Hurricane Nicole which slammed into Bermuda yesterday, Oct. 13, packing winds of about 125 mph, and is home to a critical NASA launch tracking station.

After the storm passed, engineers found the tracking station only suffered minor damage – so the GO was given to proceed with preparation for Sunday’s nighttime launch.

“Repairs to the station have been made and the team is currently readying to support the launch,” according to NASA officials.

Engineers are still testing the station to ensure its readiness.

“The Bermuda site provides tracking, telemetry and flight terminations support for Antares launches from NASA’s Wallops Flight Facility on Virginia’s Eastern Shore. Final testing is scheduled to be conducted the morning of Oct. 15 prior to the launch readiness review later that day.”

The Orbital ATK Antares rocket, with the Cygnus spacecraft onboard, is rolled out of the Horizontal Integration Facility (HIF) to begin the approximately half-mile journey to launch Pad-0A, Thursday, Oct. 13, 2016 at NASA's Wallops Flight Facility in Virginia. Orbital ATK’s sixth contracted cargo resupply mission with NASA to the International Space Station.  Credit: (NASA/Bill Ingalls)
The Orbital ATK Antares rocket, with the Cygnus spacecraft onboard, is rolled out of the Horizontal Integration Facility (HIF) to begin the approximately half-mile journey to launch Pad-0A, Thursday, Oct. 13, 2016 at NASA’s Wallops Flight Facility in Virginia. Orbital ATK’s sixth contracted cargo resupply mission with NASA to the International Space Station. Credit: (NASA/Bill Ingalls)

If all goes well Antares is sure to provide a dazzling nighttime skyshow from NASA’s Virginia launch base Sunday night – and potentially offering a thrilling spectacle to millions of US East Coast spectators.

The launch window last five minutes and the weather outlook is currently favorable.

The launch will air live on NASA TV and the agency’s website beginning at 7 p.m. EDT Oct 16.

Antares rocket stands erect, reflecting off the calm waters the night before a launch from NASA’s Wallops Flight Facility, VA, on Oct. 28, 2014.    Credit: Ken Kremer/kenkremer.com
Antares rocket stands erect, reflecting off the calm waters the night before a launch from NASA’s Wallops Flight Facility, VA, on Oct. 28, 2014. Credit: Ken Kremer/kenkremer.com

The 133-foot-tall (40-meter) Antares was rolled out to pad 0A on Thursday, Oct. 13 – three days prior to the anticipated launch date – and raised to the vertical launch position this afternoon.

The two stage Antares will carry the Orbital OA-5 Cygnus cargo freighter to orbit on a flight bound for the ISS and its multinational crew of astronauts and cosmonauts.

On-Ramp to the Orbital Sciences Antares rocket and International Space Station - ready for blastoff from NASA Wallops in this file photo.  Credit: Ken Kremer – kenkremer.com
On-Ramp to the Orbital Sciences Antares rocket and International Space Station – ready for blastoff from NASA Wallops in this file photo. Credit: Ken Kremer – kenkremer.com

The launch marks the first nighttime liftoff of the Antares – and it could be visible up and down the eastern seaboard if weather and atmospheric conditions cooperate to provide a spectacular viewing opportunity to the most populated region in North America.

The 14 story tall commercial Antares rocket also will launch for the first time in the upgraded 230 configuration – powered by new Russian-built first stage engines.

Orbital ATK’s Antares commercial rocket had to be overhauled with the completely new RD-181 first stage engines – fueled by LOX/kerosene – following the destruction of the Antares rocket and Cygnus supply ship two years ago.

The RD-181 replaces the previously used AJ26 engines which failed moments after liftoff during the last launch on Oct. 28, 2014 resulting in a catastrophic loss of the rocket and Cygnus cargo freighter.

The launch mishap was traced to a failure in the AJ26 first stage engine turbopump and caused Antares launches to immediately grind to a halt.

The new RD-181 engines are installed on the Orbital ATK Antares first stage core ready to support a full power hot fire test at the NASA Wallops Island launch pad in March 2016.  New thrust adapter structures, actuators, and propellant feed lines are incorporated between the engines and core stage.   Credit: Ken Kremer/kenkremer.com
The new RD-181 engines are installed on the Orbital ATK Antares first stage core ready to support a full power hot fire test at the NASA Wallops Island launch pad in March 2016. New thrust adapter structures, actuators, and propellant feed lines are incorporated between the engines and core stage. Credit: Ken Kremer/kenkremer.com

For the OA-5 mission, the Cygnus advanced maneuvering spacecraft will be loaded with approximately 2,400 kg (5,290 lbs.) of supplies and science experiments for the International Space Station (ISS).

“Cygnus is loaded with the Saffire II payload and a nanoracks cubesat deployer,” Frank DeMauro, Orbital ATK Cygnus program manager, told Universe Today in a interview.

Among the science payloads aboard the Cygnus OA-5 mission is the Saffire II payload experiment to study combustion behavior in microgravity. Data from this experiment will be downloaded via telemetry. In addition, a NanoRack deployer will release Spire Cubesats used for weather forecasting. These secondary payload operations will be conducted after Cygnus departs the space station.

Other experiments include a study on the effect of lighting on sleep and daily rhythms, collection of health-related data, and a new way to measure neutrons.

Watch for Ken’s continuing Antares/Cygnus mission and launch reporting. He will be reporting from on site at NASA’s Wallops Flight Facility, VA during the launch campaign.

Orbital Sciences Antares rocket explodes moments after blastoff from NASA’s Wallops Flight Facility, VA, on Oct. 28, 2014, at 6:22 p.m. Credit: Ken Kremer – kenkremer.com
Orbital Sciences Antares rocket explodes moments after blastoff from NASA’s Wallops Flight Facility, VA, on Oct. 28, 2014, at 6:22 p.m. Credit: Ken Kremer – kenkremer.com

The Cygnus spacecraft for the OA-5 mission is named the S.S. Alan G. Poindexter in honor of former astronaut and Naval Aviator Captain Alan Poindexter.

Under the Commercial Resupply Services (CRS) contract with NASA, Orbital ATK will deliver approximately 28,700 kilograms of cargo to the space station. OA-5 is the sixth of these missions.

The Orbital ATK Antares rocket, with the Cygnus spacecraft aboard. Credit: NASA/Bill Ingalls
The Orbital ATK Antares rocket, with the Cygnus spacecraft aboard. Credit: NASA/Bill Ingalls

Stay tuned here for Ken’s continuing Earth and Planetary science and human spaceflight news.

Ken Kremer

The Hidden Glaciers Of Mars

Colour-coded topographic view of the Colles Nili region, showing the relative heights and depths of terrain. Credit: ESA/DLR/FU Berlin

In the northern hemisphere of Mars, between the planet’s southern highlands and the northern lowlands, is a hilly region known as Colles Nilli. This boundary-marker is a very prominent feature on Mars, as it is several kilometers in height and surrounded by the remains of ancient glaciers.

And thanks to the Mars Express mission, it now looks like this region is also home to some buried glaciers. Such was the conclusion after the orbiting spacecraft took images that revealed a series of eroded blocks along this boundary, which scientists have deduced are chunks of ice that became buried over time.

The Mars Express images show a plethora of these features along the north-south boundary. They also reveal several features that hint at the presence of buried ice and erosion – such as layered deposits as well as ridges and troughs. Similar features are also found in nearby impact craters. All of these are believed to have been caused by an ancient glacier as it retreated several hundred million years ago.

Artist's impression of the Mars Express spacecraft in orbit. Image Credit: ESA/Medialab
Artist’s impression of the Mars Express spacecraft in orbit. Credit: ESA/Medialab

It is further reasoned that these remaining ice deposits were covered by debris that was deposited from the plateau as it eroded. Wind-borne dust was also deposited over time, which is believed to be the result of volcanic activity. This latter source is evidenced by steaks of dark material deposited around the blocks, as well as dark sand dunes spotted within the impact craters.

Similar features are believed to exist within many boundary regions on Mars, and are believed to represent periods of glaciation that took place over the course of eons. And this is not the first time buried glaciers have been spotted on Mars.

For instance, back in 2008, the Mars Reconnaissance Orbiter (MRO) used its ground-penetrating radar to locate water ice under blankets or rocky debris, and at latitudes far lower than any that had been previously identified. At the time, this information shed light on a long-standing mystery about Mars, which was the presence of what are called “aprons”.

These gently-sloping rocky deposit, which are found at the bases of taller features, were first noticed by NASA’s Viking orbiters during the 1970s. A prevailing theory has been that these aprons are the result of rocky debris lubricated by small amounts of ice.

Artist's impression visualising the separation of the ExoMars entry, descent and landing demonstrator module, Schiaparelli, from the Trace Gas Orbiter (TGO). Credit: ESA
Artist’s impression of the separation of the ExoMars entry, descent and landing demonstrator module (Schiaparelli) from the Trace Gas Orbiter (TGO). Credit: ESA/ATG medialab

Combined with this latest info taken from the northern hemisphere, it would appear that there is plenty of ice deposits all across the surface of Mars. The presence (and prevalence) of these icy remnants offer insight into Mars’ geological past, which – like Earth – involved some “ice ages”.

The Mars Express mission has been actively surveying the surface of Mars since 2003. On October 19th, it will be playing a vital role as the Exomars mission inserts itself into Martian orbit and the Schiaparelli lander makes its descent and landing on the Martian surface.

Alongside the MRO and the ExoMars Orbiter, it will be monitoring signals from the lander to confirm its safe arrival, and will relay information sent from the surface during the course of its mission.

The ESA will be broadcasting this event live. And given that this mission will be the ESA’s first robotic lander to reach Mars, it should prove to be an exciting event!

Further Reading: ESA

The Universe’s Galaxy Population Just Grew Tenfold

New research indicates that there could be as many as 2 trillion galaxies in the known Universe. Credit: 2MASS/Caltech

Ever since human beings learned that the Milky Way was not unique or alone in the night sky, astronomers and cosmologists have sought to find out just how many galaxies there are in the Universe. And until recently, our greatest scientific minds believed they had a pretty good idea  – between 100 and 200 billion.

However, a new study produced by researchers from the UK has revealed something startling about the Universe. Using Hubble’s Deep Field Images and data from other telescopes, they have concluded that these previous estimates were off by a factor of about 10. The Universe, as it turns out, may have had up to 2 trillion galaxies in it during the course of its history.

Led by Prof. Christopher Conselice of the University of Nottingham, U.K., the team combined images taken by the Hubble Space Telescope with other published data to produced a 3-D map of the Universe. They then incorporated a series of new mathematical models that allowed them to infer the existence of galaxies which are not bright enough to be observed by current instruments.

Scientists believe they have found the missing matter of the universe, thus confirming our current cosmological models. Credit: NASA/Chandra
Scientists from the UK have produced new estimates on the number of galaxies in the Universe, which could shed light on cosmic evolution as well. Credit: NASA/Chandra

Using these, they then began reviewing how galaxies have evolved over the past 13 billion years. What they learned was quite fascinating. For one, they observed that the distribution of galaxies throughout the history of the Universe was not even. What’s more, they found that in order for everything in their calculations to add up, there had to be 10 times more galaxies in the early Universe than previously thought.

Most of these galaxies would be similar in mass to the satellite galaxies that have been observed around the Milky Way, and would be too faint to be spotted by today’s instruments. In other words, astronomers have only been able to see about 10% of the early Universe until now, because most of its galaxies were too small and faint to be visible.

As Prof. Conselice explained in a Hubble Science Release, while may help resolve a lingering debate about the structure of the Universe:

“These results are powerful evidence that a significant galaxy evolution has taken place throughout the universe’s history, which dramatically reduced the number of galaxies through mergers between them — thus reducing their total number. This gives us a verification of the so-called top-down formation of structure in the universe.”

Illustration of the depth by which Hubble imaged galaxies in prior Deep Field initiatives, in units of the Age of the Universe. The goal of the Frontier Fields is to peer back further than the Hubble Ultra Deep Field and get a wealth of images of galaxies as they existed in the first several hundred million years after the Big Bang. Note that the unit of time is not linear in this illustration. Illustration Credit: NASA and A. Feild (STScI)
Illustration of the depth by which Hubble imaged galaxies in prior Deep Field initiatives, in units of the Age of the Universe. Credit: NASA and A. Feild (STScI)

To break it down, the “top-down model” of galaxy formation states that galaxies formed from huge gas clouds larger than the resulting galaxies. These clouds began collapsing because their internal gravity was stronger than the pressures in the cloud. Based on the speed at which the gas clouds rotated, they would either form a spiral or an  elliptical galaxy.

In contrast, the “bottom-up model” states that galaxies formed during the early Universe due to the merging of smaller clumps that were about the size globular clusters. These galaxies could then have been drawn into clusters and superclusters by their mutual gravity.

In addition to helping to resolve this debate, this study also offers a possible solution to the Olbers’ Paradox (aka. “the dark night sky paradox”). Named after the 18th/19th century German astronomer Heinrich Wilhelm Olbers, this paradox addresses the question of why – given the expanse of the Universe and all the luminous matter in it – is the sky dark at night?

Based on their results, the UK team has surmised that while every point in the night sky contains part of a galaxy, most of them are invisible to the human eye and modern telescopes. This is due to a combination of factors, which includes the effects of cosmic redshift, the fact that the Universe is dynamic (i.e. always expanding) and the absorption of light by cosmic dust and gas.

Among other data, scientists used the galaxies visible in the Great Observatories Origins Deep Survey (GOODS) to recalculate the total number of galaxies in the observable Universe. The image was taken by the NASA/ESA Hubble Space Telescope and covers a portion of the southern field of GOODS. This is a large galaxy census, a deep-sky study by several observatories to trace the formation and evolution of galaxies.
Image was taken by the NASA/ESA Hubble Space Telescope which covers a portion of the southern field of Great Observatories Origins Deep Survey (GOODS). Credit: NASA/ESA/HST

Needless to say, future missions will be needed to confirm the existence of all these unseen galaxies. And in that respect, Conselice and his colleagues are looking to future missions – ones that are capable of observing stars and galaxies in the non-visible spectrum – to make that happen.

“It boggles the mind that over 90 percent of the galaxies in the universe have yet to be studied,” he added. “Who knows what interesting properties we will find when we discover these galaxies with future generations of telescopes? In the near future, the James Webb Space Telescope will be able to study these ultra-faint galaxies.”

Understanding how many galaxies have existed over time is a fundamental aspect of understanding the Universe as a whole. With every passing study that attempts to resolve what we can see with our current cosmological models, we are getting that much closer!

And be sure to enjoy this video about some of Hubble’s most stunning images, courtesy of HubbleESA:

Further Reading: HubbleSite, Hubble Space Telescope

Weekly Space Hangout – October 14, 2016: Europe Crashes the Mars Party

Host: Fraser Cain (@fcain)

Special Guest:

Guests:
Tyler Finlay of the Sally Ride EarthKAM project

Guests:
Morgan Rehnberg (MorganRehnberg.com / @MorganRehnberg)

Their stories this week:
Two trillion galaxies?

Obama reaffirms NASA’s Mars plan

ExoMars arrives in the coming week

CosmoQuest Survey for Citizen Scientists – how can we make citizen science more available?

CosmoQuest Survey for Parents who have kids doing Science Fair Projects – how can we help you?

CosmoQuest Survey for Teachers assigning Science Fair Projects – how can we help you?

We use a tool called Trello to submit and vote on stories we would like to see covered each week, and then Fraser will be selecting the stories from there. Here is the link to the Trello WSH page (http://bit.ly/WSHVote), which you can see without logging in. If you’d like to vote, just create a login and help us decide what to cover!

If you would like to join the Weekly Space Hangout Crew, visit their site here and sign up. They’re a great team who can help you join our online discussions!

If you would like to sign up for the AstronomyCast Solar Eclipse Escape, where you can meet Fraser and Pamela, plus WSH Crew and other fans, visit our site linked above and sign up!

We record the Weekly Space Hangout every Friday at 12:00 pm Pacific / 3:00 pm Eastern. You can watch us live on Universe Today, or the Universe Today YouTube page.

We Land on Mars in Just 2 days!

Artist's view of the Schiaparelli lander descending to Mars on October 19. Credit: ESA


Watch how Schiaparelli will land on Mars. Touchdown will occur at 10:48 a.m. EDT (14:48 GMT) Wednesday Oct. 19.

Cross your fingers for good weather on the Red Planet on October 19. That’s the day the European Space Agency’s Schiaparelli lander pops open its parachute, fires nine, liquid-fueled thrusters and descends to the surface of Mars. Assuming fair weather, the lander should settle down safely on the wide-open plains of Meridiani Planum near the Martian equator northwest of NASA’s Opportunity rover. The region is rich in hematite, an iron-rich mineral associated with hot springs here on Earth.

On 19 October 2016, the ExoMars 2016 entry, descent, and landing demonstrator module, known as Schiaparelli, will land on Mars in a region known as Meridiani Planum. The landing sites of the seven rovers and landers that have reached the surface of Mars and successfully operated there are indicated on this map. The background image is a shaded relief map of Mars, based on data from the Mars Orbiter Laser Altimeter (MOLA) instrument, on NASA’s Mars Global Surveyor spacecraft.
On Wednesday, October 19, the ExoMars 2016 entry, descent and landing demonstrator module, named Schiaparelli, will land on Mars in Meridiani Planum not far from the Opportunity rover. The map shows the seven rovers and landers that have reached the surface of Mars and successfully operated there. The background image is a shaded relief map of Mars created using data from NASA’s Mars Global Surveyor spacecraft.

The 8-foot-wide probe will be released three days earlier from the Trace Gas Orbiter (TGO) and coast toward Mars before entering its atmosphere at 13,000 mph (21,000 km/hr). During the 6-minute-long descent, Schiaparelli will decelerate gradually using the atmosphere to brake its speed, a technique called aerobraking. Not only is Meridiani Planum flat, it’s low, which means the atmosphere is thick enough to allow Schiaparelli’s heat shield to reduce its speed sufficiently so the chute can be safely deployed. The final firing of its thrusters will ensure a soft and controlled landing.

Artist's impression depicting the separation of the ExoMars 2016 entry, descent and landing demonstrator module, named Schiaparelli, from the Trace Gas Orbiter, and heading for Mars. Credit: ESA/ATG medialab
Artist’s impression showing Schiaparelli separating from the Trace Gas Orbiter and heading for Mars. The lander is named for late 19th century Italian astronomer Giovanni Schiaparelli, who created a detailed telescopic map of Mars. The orbiter will sniff out potentially biological gases such as methane in Mars’ atmosphere and track its sources and seasonal variations. Credit: ESA/ATG medialab

The lander is one-half of the ExoMars 2016 mission, a joint venture between the European Space Agency and Russia’s Roscosmos. The Trace Gas Orbiter (TGO) will fire its thrusters to place itself in orbit about the Red Planet the same day Schiparelli lands. Its job is to inventory the atmosphere in search of organic molecules, methane in particular. Plumes of methane, which may be biological or geological (or both) in origin, have recently been detected at several locations on Mars including Syrtis Major, the planet’s most prominent dark marking. The orbiter will hopefully pinpoint the source(s) as well as study seasonal changes in locations and concentrations.

This image, taken by the High Resolution Stereo Camera (HRSC) on board ESA’s Mars Express spacecraft, shows what appears to be a dust-covered frozen sea near the Martian equator. It shows a flat plain, part of the Elysium Planitia, that is covered with irregular blocky shapes. They look just like the rafts of fragmented sea ice that lie off the coast of Antarctica on Earth. Raised levels of methane were detected here by ESA's Mars Express orbiter. Copyright: ESA/DLR/FU Berlin (G. Neukum)
This image, taken by ESA’s Express spacecraft, shows what appears to be a dust-covered frozen sea near the Martian equator. Located in Elysium Planitia, the flat plain is covered with irregular blocky shapes. They look just like the rafts of fragmented sea ice that lie off the coast of Antarctica on Earth. Raised levels of methane were detected here by ESA’s Mars Express orbiter. Copyright: ESA/DLR/FU Berlin (G. Neukum)

Methane (CH4) has long been associated with life here on Earth. More than 90% of the colorless, odorless gas is produced by living organisms, primarily bacteria. Sunlight breaks methane down into other gases over a span of about 300 years. Because the gas relatively short-lived, seeing it on Mars implies an active, current source. There may be several:

  • Long-extinct bacteria that released methane that became trapped in ice or minerals in the upper crust. Changing temperature and pressure could stress the ice and release that ancient gas into today’s atmosphere.
  • Bacteria that are actively producing methane to this day.
  • Abiological sources. Iron can combine with oxygen in terrestrial hot springs and volcanoes to create methane. This gas can also become trapped in solid forms of water or ‘cages’ called clathrate hydrates that can preserve it for a long time. Olivine, a common mineral on Earth and Mars, can react with water under the right conditions to form another mineral called serpentine. When altered by heat, water and pressure, such in environments such as hydrothermal springs, serpentine can produce methane.

Will it turn out to be burping bacteria or mineral processes? Let’s hope TGO can point the way.

This image illustrates possible ways methane might get into Mars’ atmosphere and also be removed from it: microbes (left) under the surface that release the gas into the atmosphere, weathering of rock (right) and stored methane ice called a clathrate. Ultraviolet light can work on surface materials to produce methane as well as break it apart into other molecules (formaldehyde and methanol) to produce carbon dioxide. Credit: NASA/JPL-Caltech/SAM-GSFC/Univ. of Michigan
This image illustrates possible ways methane might get into Mars’ atmosphere and also be removed from it: microbes (left) under the surface that release the gas into the atmosphere, weathering of rock (right) and stored methane ice called a clathrate. Ultraviolet light can work on surface materials to produce methane as well as break it apart into other molecules (formaldehyde and methanol) to produce carbon dioxide. Credit: NASA/JPL-Caltech/SAM-GSFC/Univ. of Michigan

The Trace Gas Orbiter will also use the Martian atmosphere to slow its speed and trim its orbital loop into a 248-mile-high (400 km) circle suitable for science observations. But don’t expect much in the way of scientific results right away; aerobraking maneuvers will take about a year, so TGO’s job of teasing out atmospheric ingredients won’t begin until December 2017. The study runs for 5 years.

The orbiter will also examine Martian water vapor, nitrogen oxides and other organics with far greater accuracy than any previous probe as well as monitor seasonal changes in the atmosphere’s composition and temperature. And get this — its instruments can map subsurface hydrogen, a key ingredient in both water and methane, down to a depth of a meter (39.4 inches) with greater resolution compared to previous studies. Who knows? We may discover hidden ice deposits or methane sinks that could influence where future rovers will land. Additional missions to Mars are already on the docket, including ExoMars 2020. More about that in a minute.

Schiaparelli, the
This artist’s view shows Schiaparelli, the entry, descent and landing demonstrator module, using its thrusters to make a soft landing on Mars on October 19 at 10:48 a.m. EDT (14:48 GMT). Credit: ESA/ATG medialab

While TGO’s mission will require years, the lander is expected to survive for only four Martian days (called ‘sols’) by using the excess energy capacity of its batteries. A set of scientific sensors will measure wind speed and direction, humidity, pressure and electric fields on the surface. A descent camera will take pictures of the landing site on the way down; we’ll should see those photos the very next day. Data and imagery from the lander will be transmitted to ESA’s Mars Express and a NASA Relay Orbiter, then relayed to Earth.


This animation shows the paths of the Trace Gas Orbiter and Schiaparelli lander on Oct. 19 when they arrive at Mars.

If you’re wondering why the lander’s mission is so brief, it’s because Schiaparelli is essentially a test vehicle. Its primary purpose is to test technologies for landing on Mars including the special materials used for protection against the heat of entry, a parachute system, a Doppler radar device for measuring altitude and liquid-fueled braking thrusters.

Martian dust storms can be cause for concern during any landing attempt. Since it’s now autumn in the planet’s northern hemisphere, a time when storms are common, there’s been some finger-nail biting of late. The good news is that storms of recent weeks have calmed and Mars has entered a welcome quiet spell.

To watch events unfold in real time, check out ESA’s live stream channel, Facebook page and Twitter updates. The announcement of the separation of the lander from the orbiter will be made around 11 a.m. Eastern Time (15:00 GMT) Sunday October 16.  Live coverage of the Trace Gas Orbiter arrival and Schiaparelli landing on Mars runs from 9-11:15 a.m. Eastern (13:00-15:15 GMT) on Wednesday October 19. Photos taken by Schiaparelli’s descent camera will be available starting at 4 a.m. Eastern (8:00 GMT) on October 20. More details here. We’ll also keep you updated on Universe Today.

The ExoMars 2016 mission will pave the way for a rover mission to the Red Planet in 2020. Credit: ESA
The ExoMars 2016 mission will pave the way for a rover mission to the Red Planet in 2020. Credit: ESA

Everything we learn during the current mission will be applied to planning and executing the next —  ExoMars 2020, slated to launch in 2020. That venture will send a rover to the surface to search and chemically test for signs of life, present or past.  It will collect samples with a drill at various depths and analyze the fines for bio-molecules. Getting down deep is important because the planet’s thin atmosphere lets through harsh UV light from the sun, sterilizing the surface.

Are you ready for adventure? See you on Mars (vicariously)!