Tag Archives: Observations

An active asteroid

Hi there! Today we will detail a recent study by Jessica Agarwal and Michael Mommert, entitled Nucleus of active asteroid 358P/Pan-STARRS (P/2012 T1). This study has recently been accepted for publication in Astronomy and Astrophysics, and consists in increasing our knowledge of a recently discovered object, i.e. P/2012 T1. This object proved to have some activity, like a comet. The authors realized several observations to try to characterize its activity, and infer some physical properties like its size and its rotation.

Comet vs. active asteroid

First of all, I would like to make clear what is a comet, and what is an active asteroid. I am very ambitious here, since these two notions actually overlap. For instance, our object is both an active asteroid, and a main-belt comet.

Let us say that a comet is an active asteroid, while an active asteroid is not necessarily a comet. The difference is in the nature of the activity.

A comet is a dirty snowball, i.e. you have water ice, and some silicates. Its orbit around the Sun is usually pretty eccentric, so that you have large variations of the distance Sun-object. The location of the orbit, at which the distance is the smallest, is called pericentre. When the comet approaches the pericentre, it approaches the Sun, heats, and part of its water ice sublimates. This results in a dusty tail (actually there are two tails, one being composed of ionized particles).

But when you see dust around a small body, i.e. when you see activity, this is not necessarily ice sublimation. There could be for instance rock excavated by an impact, or material expelled by fast rotation. In that case, you still have an active asteroid, but not a comet. One of the goals of this study is to address the cause and nature of P/2012 T1’s activity.

The asteroid P/2012 T1

P/2012 T1, now named 358P, has been discovered in October 2012 by the Pan-STARRS-1 survey. Pan-STARRS stands for Panoramic Survey Telescope and Rapid Response System, it uses dedicated facilities at Haleakala Observatory, Hawaii, USA.

Discovery of P/2012 T1. © Pan-STARRS
Discovery of P/2012 T1. © Pan-STARRS

Its provisional name, P/2012 T1, contains information on the nature of the object, and its discovery. P stands for periodic comet, 2012 is the year of the discovery, and T means that it has been discovered during the first half of October.

Interestingly, this object appeared on images taken in December 2001 at Palomar Observatory in California, while acquiring data for the survey NEAT (Near-Earth Asteroid Tracking).

You can find below its orbital elements, from the Minor Planet Center:

Semi-major axis 3.1504519 AU
Eccentricity 0.2375768
Inclination 11.05645°
Period 5.59 y

From its orbital dynamics, it is a Main-Belt object. As a comet, it is a Main-Belt Comet.

New observations

Once an object is known and we know where it is, it is much easier to reobserve it. The authors conducted observations of 358P from the Southern Astrophysical Research (SOAR) telescope, and the Very Large Telescope.

The SOAR telescope is based on Cerro Pachón, Chile. This is a 4.1-m aperture facility, located at an altitude of 2,700 m. The authors took images with the Goodman High Throughput Spectrograph during one night, from July 27 to July 28, 2017. They wanted to analyze the reflected light by the asteroid at different wavelengths, unfortunately the observational constraints, i.e. cloud coverage, permitted only two hours of observations. Only the observations made with the VR filter, centered at 610 nm, were useful.

These data were supplemented by 77 images taken during 10 hours from August 17 to August 18, 2017, at the Very Large Telescope. This instrument depends on the European Southern Observatory (ESO), and is located on Cerro Paranal, once more in Chile, at an altitude of 2,635 m. The authors used the FOcal Reducer and low dispersion Spectrograph 2 (FORS2), which central wavelength is 655 nm.

The observations give raw images. The authors treated them to get reliable photometric and astrometric measurements of 358P, i.e. they corrected from the variations of the luminosity of the sky, in using reference stars, and from the possible instrumental problems. For that, they recorded the response of the instrument to a surface of uniform brightness, and used the outcome to correct their images.

Let us now address the results.

Measuring its rotation

Such a small (sub-kilometric) body is not spherical. This results in variations of luminosity, which depend on the surface element which is actually facing your telescope. If you acquire data during several spin periods of the asteroid, then you should see some periodicity in the recorded lightcurve.

The best way to extract the periods is to make a Fourier transform. Your input is the time-dependent lightcurve you have recorded, and your output is a frequency-dependent curve, which should emphasize the periods, which are present in the recorded lightcurve. If the signal is truly periodic, then it should exhibit a maximum at its period and its harmonics (i.e. twice the period, thrice the period, etc.), and almost 0 outside (not exactly 0 since you always have some noise).

In the case of 358P, the authors did not identify any clear period. A maximum is present for a rotation period of 8 hours, but the result is too noisy to be conclusive. A possible explanation could be that we have a polar view of the asteroid. Another possibility is that the albedo of the asteroid (the fraction of reflected light) is almost uniform.

Dust emission

The authors tried to detect debris around the nucleus of the comet, in widening the aperture over which the photometry was performed. They got no real detection, which tends to rule out the possibility of non-cometary activity.

A 530m-large body

Finally, the magnitude of the asteroid is the one of a sphere of 530 meters in diameter, with an albedo of 6%. This means that a higher albedo would give a smaller size, and conversely. The albedo depends on the composition of the asteroid, which is unknown, and can be only inferred from other asteroids. The authors assumed it to be a carbonaceous asteroid (C-type), as 75% of the asteroids. If it were an S-type (silicateous) body, then it would be brighter. A wide band spectrum of the reflected light would give us this information.

The study and its authors

  • You can find the study here, on Astronomy and Astrophysics’ website. Moreover, the authors uploaded a free version on arXiv, thanks to them for sharing!
  • Here is the webpage of the first author, Jessica Agarwal,
  • and here the website of Michael Mommert.

And that’s it for today! Please do not forget to comment. You can also subscribe to the RSS feed, and follow me on Twitter, Facebook, Instagram, and Pinterest.

Uranus’s satellites are red

Hi there! Today, we speak about the satellites of Uranus. They have been visited only once by a spacecraft, i.e. Voyager 2 in 1986, but we dispose of Earth-based facilities, which are able to give us some clues. The study I present today, Red material on the large moons of Uranus: Dust from irregular satellites? discusses the fact that the main moons appear to be redder than the large moons of Jupiter and Saturn.

Let me define redder first: the surface of these bodies reflects the Solar incident light. A spectral decomposition of the reflected light tells us something on the material coating the surface. And the relative response of the surface in the different wavelengths is higher in the infrared for the large moons of Uranus, than it is for the moons of Jupiter and Saturn.

This study, by Richard Cartwright et al., has recently been published in Icarus.

The satellites of Uranus

First: Uranus. This is the seventh planet of our Solar System, which orbits in 84 years, and which seems to roll on its orbit. Actually, its rotation axis is tilted by nearly 90° (actually 97.8°), and its main satellites and rings orbit close to its equatorial plane. Their orbits are tilted as well.

The satellites of Uranus, all named after Shakespeare’s characters, can be categorized into 3 groups:

  1. The 13 small, inner satellites, which are embedded into the rings,
  2. the 5 main ones,
  3. and the 9 irregular satellites, which orbit much further from Uranus, and which orbits may be tilted. Contrary to the other two groups, they have probably not been formed in the proto-Uranus nebula, but were former asteroids, which have been trapped by Uranus.

You can find below some properties and orbital characteristics of the main satellites. All of these bodies have been discovered from the Earth. These are the targets of the study I present.

Discovery Semimajor axis Eccentricity Inclination Orbital period Mean diameter
Miranda 1948 129,900 km 0.0013 4.338° 1.413 d 471.6 km
Ariel 1851 190,900 km 0.0012 0.041° 2.520 d 1,157.8 km
Umbriel 1851 266,000 km 0.0039 0.128° 4.144 d 1,169.4 km
Titania 1787 436,300 km 0.0011 0.079° 8.706 d 1,577.8 km
Oberon 1787 583,500 km 0.0014 0.068° 13.46 d 1,522.8 km

You can see that they have limited eccentricities and inclinations, except for the inclination of Miranda, which probably results from a past resonant forcing by Umbriel. In the past, the orbital period of Umbriel was exactly thrice the one of Miranda, and this has forced its inclination, which was thus initially very small. Anyway, it remains close to the equatorial plane for Uranus.

You can see below that things are different for the small satellites.

Discovery Semimajor axis Eccentricity Orbital period Mean diameter
Francisco 2001 4,282,900 km 0.13 267 d ≈22 km
Caliban 1997 7,231,100 km 0.18 580 d ≈72 km
Stephano 1999 8,007,400 km 0.22 677 d ≈32 km
Trinculo 2001 8,505,200 km 0.22 749 d ≈18 km
Sycorax 1997 12,179,400 km 0.52 1,288 d ≈150 km
Margaret 2003 14,146,700 km 0.68 1,661 d ≈20 km
Prospero 1999 16,276,800 km 0.44 1,978 d ≈50 km
Setebos 1999 17,420,400 km 0.59 2,225 d ≈48 km
Ferdinand 2001 20,430,000 km 0.40 2,790 d ≈20 km

These are very small bodies, which orbit very far from Uranus, on eccentric orbits. Besides, their orbital planes have just nothing to do with the equatorial plane of Uranus. This is why we believe they are former asteroids. Beside Margaret, they all orbit on retrograde orbits, while all the regular moons are prograde. Discovering them required to use telescopes of a least 5 m, the satellites discovered in 2003 having been discovered during a systematic survey with the Subaru telescope at Mauna Kea, Hawaii, over a field of 3.5 degrees. They all have apparent magnitudes larger than 20.

Only one space mission visited them: Voyager 2, in January 1986.

Voyager 2 at Uranus

The spacecraft Voyager 2 was launched from Cape Canaveral, Florida, in August 1977. It benefited from a favorable geometrical configuration of the 4 giant planets to visit all of them. Unfortunately, this required the spacecraft to travel too fast to permit an orbital insertion. So, contrary to Cassini which toured around Saturn during 13 years, Voyager 2 just passed by.

Its closest approach to Uranus was on January 24, 1986, at a distance of 81,500 km from the planet’s cloud tops. It permitted the discovery of 11 inner satellites, and partly imaged the large ones. It revealed in particular geological features on Miranda, and analyzed the light reflected by the surface of these bodies. The study we discuss today supplements these measurements.

Miranda seen by Voyager 2. © NASA/JPL/USGS
Miranda seen by Voyager 2. © NASA/JPL/USGS

Observations at IRTF

The authors used NASA’s InfraRed Telescope Facility (IRTF). This is a 3-meter telescope, optimized for infrared astronomy. It is located at the Mauna Kea Observatory (altitude: 4,200 m) in Hawaii (USA), and 50% of the observation time is devoted to planetary observation.
Several instruments are available, the authors used the spectrograph-imager SpeX, which decomposes the incident light between 0.8 and 5.4 µm. In that study, the authors limited to 4.2 µm.

NASA's InfraRed Telescope Facility at Maune Kea, Hawaii. © Afshin Darian
NASA’s InfraRed Telescope Facility at Maune Kea, Hawaii. © Afshin Darian

The outcome of such observations is a plot amplitude vs. wavelength of a given surface element of a satellite. It is interesting to keep in mind that the regular moons rotate synchronously, permanently showing the same face to Uranus. The consequence is that they have a leading and a trailing hemisphere. During their orbital motion, the same hemisphere always leads. And this has implications for the surface composition, because the leading hemisphere can be polluted by the dusty environment. In other words: when you observe something on the leading hemisphere, which is not present on the trailing one, this is probably pollution.

When you observe, you actually observe the surface element which faces you. And this depends on the dynamics of the planet.

Geometrical constraints

As you know, Uranus rolls on its orbit, while the satellites have an equatorial orbit. As a consequence, during a 84-y orbit of Uranus around the Sun, the Earth crosses twice the orbital plane, and two periods are favorable for the observation of the poles of Uranus and the satellites. The northern hemispheres of these bodies face us during half the orbit (42 years), while the southern ones face us during the other half.

The last transition happened in 2007. Since then, the northern hemispheres of the satellites face us. And part of the visible face belongs to the leading hemisphere.

A red leading side

The results show that for Ariel and Umbriel, and even more for Titania and Oberon, the leading hemisphere is significantly redder than the trailing one, while it is not the case for the major satellites of Jupiter and Saturn. Titania and Oberon are the outermost of the satellites of Uranus, and the largest ones as well.

To understand the chemical nature of this reddening, previous studies have conducted lab experiments, consisting in reproducing the spectrum of mixtures of chemical elements, which could be found on the natural satellites of the outer planets. Of course, the conditions of temperature and pressure are considered. Then the spectrums are compared to the actually observed ones. And it appears that the reddening agents should be tholins and pyroxene.

Titania seems to have a red spot on its surface, which makes it the redder of the main Uranian satellites. Contrariwise, Miranda does not present this reddening. Latitudinal variations of color are not obvious, while they are in longitude, since they depend on the leading / trailing effect.

Now, the question is: how did these agents reach the satellites? They are probably not endogenous, since similar satellites around Jupiter and Saturn do not have them.

Pollution by the irregular moons

The smoking gun is the irregular moons: they are pretty red. And numerical simulations of the motion of dust expelled from these satellites by impacts show how they are likely to coat the leading sides of Oberon, Titania, Ariel and Umbriel.
And this is what we observe!

Of course, a space mission to Uranus would be very helpful… but this is another story.

The study and its authors

And that’s it for today! Please do not forget to comment. You can also subscribe to the RSS feed, and follow me on Twitter, Facebook, Instagram, and Pinterest.

Triton from the Earth

Hi there! Today we speak about Triton. Triton is something unique in the Solar System. It is a large satellite of Neptune, which has almost no mid-sized satellite, contrary to Saturn and Uranus. Several studies show us that Triton could have been a cuckoo, i.e. initially a Trans-Neptunian Objects, which has been trapped by the gravitational field of Neptune, and which is massive enough to have ejected the mid-sized satellites.
Triton has been visited only once, by NASA’s Voyager 2 in 1989. This was only a fly-by, so we have images of only 40% of the surface. But the development of Earth-based instruments now permits to get data from the Earth, even if the apparent magnitude of Triton is 13.47 (Neptune is very far away…).

This is the opportunity to present Triton’s surface ices: Distribution, temperature and mixing state from VLT/SINFONI observations, by F. Merlin, E. Lellouch, E. Quirico and B. Schmitt, all based in France, even if they used European facilities based in Chile. This study has recently been accepted for publication in Icarus.

Triton’s facts

The table below gives you some numbers.

Discovery 1846
Radius 1,353 km
Semimajor axis 354,759 km
Orbital period 5.88 days
Eccentricity 2×10-5
Inclination 157°

You can see first that Triton has been discovered in October 1846, by the British astronomer William Lassell. The discovery happened 10 days after the discovery of Neptune, and this is of course not by chance. When the discovery of a planet is made and announced, it is much easier, or much less difficult, to re-observe it, since you know where to point your telescope. So, Neptune has been reobserved, and Lassell saw this point following Neptune. You can distinguish a satellite from a background star by the fact that the satellite follows the planet in its apparent motion. This was Triton. And Triton was the only known satellite of Neptune during more than one century, until the discovery of Nereid by Gerard Kuiper in 1949.

As I said, Triton is pretty large, and its orbit is almost circular, as for many natural satellites of the giant planets. The tidal interaction with the parent planet tends to circularize the orbit, unless the eccentricity is excited by the action of another satellite… which cannot be the case around Neptune, since no satellite is heavy enough to move Triton.

A trapped object…

The interesting point about the dynamics of Triton is its orbital inclination. While natural satellites usually orbit close to the equatorial plane of their planet, Triton has a very large inclination, and its orbit is retrograde with respect to the rotation of Neptune. Usually, the natural satellites are formed with the planet, in the proto-planetary nebula, which is pretty flat… this is why their inclinations should be small. The inclination of Triton suggests it was not formed in situ, but has been trapped instead. Several studies have simulated this phenomenon, see e.g. your favorite blog.

…visited by Voyager 2

NASA’s Voyager 2 has been launched in August 1977 from Cape Canaveral, and it benefited from a favorable geometrical configuration of the planets. This virtual alignment permitted to fly by Jupiter in 1979, Saturn in 1981, Uranus in 1986, and Neptune in 1989. Voyager 2 is still operating, as an interstellar mission.

Only a fly by may be frustrating, but for a spacecraft to be inserted an orbit around a planet, it must reach it slowly enough… which means take enough time to reach it. Neptune is so far away that we could not wait. So, its closest approach to Neptune was on August 25, 1989, and the closest to Triton 3 days later, imaging 40% of its surface (see video below, made by Paul Schenk, Lunar and Planetary Institute, Houston, TX, USA).

It revealed an active surface, i.e. few craters, which means that the surface is renewing, and geological features, craters, ridges, plains, maculae… and even volcanic plumes. It also confirmed the presence of an atmosphere.

The atmosphere of Triton

Triton has a very tenuous atmosphere, which pressure is 70,000 times lower than the one of the Earth, i.e. some 14 μbar. It is dominated by nitrogen, and extends 800 kilometers above its surface. Methane and carbon monoxide are also present. Its temperature is around 40 K, and Voyager 2 measured winds from the west from the surface to an altitude of 8 km, where the winds invert their directions, i.e. from east to west.

This atmosphere is probably the result of outgassing of surface material and volcanic activity (geysers). It can be seen as an equilibrium between a solid phase at the surface, and a gaseous one in the atmosphere, of some of its constituents. The study I present today analyses the chemical elements present at the surface, which interact with the atmosphere. The used facility is the instrument SINFONI, on the Very Large Telescope (Paranal Observatory, Chile).

THE VLT/SINFONI instrument

The Very Large Telescope, VLT for short, is a facility operated by the European Southern Observatory in the Atacama desert, Chile. It benefits from a very favorable sky, at an altitude of 2,635 meters, and consists of 4 refractors, Antu, Kueyen, Melipal, and Yepun, each with a primary mirror of 8.2 meters.

SINFONI, for Spectrograph for Integral Field Observations in the Near Infrared, operates on Yepun, and observes in the near-infrared, i.e. at wavelengths between 1 and 2.45 μm. You can find below its first light in July 2004, observing the star HD 130163.

"First Light" "data cube" spectrum obtained with SINFONI on the bright star HD 130163 on July 9, 2004, as seen on the science data computer screen. This 7th-magnitude A0 V star was observed in the near-infrared H-band with a moderate seeing of 0.8 arcsec. The width of the slitlets in this image is 0.25 arcsec. The exposure time was 1 second. © ESO
“First Light” “data cube” spectrum obtained with SINFONI on the bright star HD 130163 on July 9, 2004, as seen on the science data computer screen. This 7th-magnitude A0 V star was observed in the near-infrared H-band with a moderate seeing of 0.8 arcsec. The width of the slitlets in this image is 0.25 arcsec. The exposure time was 1 second. © ESO

As a spectrometer, it decomposes the light it observes following its wavelengths. You can find above a spectrum, on which you can see several minimums. These minimums are absorption lines, which reveal the presence of a chemical element. And this is the idea: the authors decomposed the Solar light reflected by the surface of Triton, to detect the chemical elements constituting it.

Spectral measurements

The authors made 5 observations between 2010 and 2013, each of them lasting between 40 and 55 minutes. They supplemented their data set with two observations dating back to 1995, and one to 2008. The 1995 observations were made at Mauna Kea Observatory, Hawaii.
Two spectral bands were investigated: the H band (1.5 to 1.8 μm) and the K band (2 to 2.45 μm). Once the data are acquired, they must be corrected from the influence of the Earth atmosphere and the one of Triton, which have themselves constituents which absorb the light. Pretty easy for correcting the telluric lines, however the authors admit that the correction from Triton’s atmosphere is not entirely satisfactory, given the accuracy of data we dispose on. In particular, this correction might add an artificial signature of methane.

After these corrections, and some that I do not detail, you have the spectra… What do to with that?

Lab experiments to understand the data

The spectrum should look like something we know. We know the absorption lines of methane, carbon monoxide, carbon dioxide, nitrogen… but not necessarily under Triton’s conditions. The temperature at the surface should be around 40 K, i.e. -235°C / -390°F, to permit the coexistence of the solid and gaseous phases of these elements, without liquid phase, with a pressure of 14μbar. And when you look at the spectrum, you do not only have the location of the absorption lines, but also their amplitudes, which depend on many parameters, like the temperature, the grain size, the relative fraction of these components, and corrections accounting for instrumental constraints.
To get these parameters, the authors made several lab experiments in Grenoble (France), got plenty of spectra, and fitted their observations of Triton on them. Actually, lab experiments have been made in the past and used to previous studies, but in the present case this wasn’t enough, given the resolution of the new data.

And now, the results!

Results

The results are essentially a confirmation of previous studies, but with a better resolution, and new data, which gives access to time variations of the composition. Actually, the variations of the distance to the Sun results in variations of temperature, which perturb the equilibrium between the solid and the gaseous phases.

Regarding the different constituents:

  • The methane (CH4) is mostly in diluted form.
  • At least two populations of carbon dioxide (CO2) are present, with grain sizes of 5 μm and 25 μm, respectively.
  • The carbon monoxide (CO) is mostly present in diluted form into nitrogen ice.
  • The nitrogen (N2) ice temperature is 37.5±1 K.

The study confirms already known longitudinal variations of the nitrogen and carbon monoxide surface abundances, and suggests latitudinal and/or temporal variations.

This may be anecdotal, but the authors have detected two unexpected absorption lines, at 2.102 μm and 2.239 μm. The first one being present in one spectrum only, while the last one is detected on the three spectra. What do they mean? We do not know yet.

So, you see, it is possible to get data on Triton from our Earth. But a space mission to Neptune would be much more fruitful. But this is a very strong challenge. Even a mission to Uranus seems to become difficult to fund. Some scientists fight for that. But anyway, do not forget that you will be much older than you are now when such a mission would reach its destination, if launched now…

The study and its authors

And that’s it for today! Please do not forget to comment. You can also subscribe to the RSS feed, and follow me on Twitter, Facebook, Instagram, and Pinterest.

There was water on Mars

Hi there! Well, we already knew that there has been liquid water on the surface of Mars, a long time ago. Indeed, the space mission Mariner 9 imaged valley networks in 1972. Since then, several missions refined the data. The study I present today, Estimate of the water flow duration in large Martian fluvial systems, by Vincenzo Orofino, Giulia Alemanno, Gaetano Di Achille and Francesco Mancarella, uses the most recent observations to estimate the length and depth of former Martian rivers, and their duration of formation and erosion. This study has recently been accepted for publication in Planetary and Space Science.

Evidences of liquid water in the past

The current atmosphere of Mars is pretty thin, its pressure being on average 0.6% the one of the Earth. Such a small atmospheric pressure prevents the existence of liquid water at the surface. Water could survive only as ice, otherwise would be just vaporized. And ice water has been found, particularly in the polar caps. But if the atmosphere were thicker in the past, then liquid water would have survived… and we know it did.

We owe to Mariner 9 a map of 85% of the Martian surface, which revealed in particular river beds, deltas, and lake basins. The study we discuss today focused on valley networks, which are particularly present in the southern highlands of Mars. These valleys are typically less than 5 km wide, but may extend over thousands of kms, and they reveal former rivers.

Nirgal Vallis seen by Mariner 9. © NASA
Nirgal Vallis seen by Mariner 9. © NASA

The history of these rivers is inseparable from the geological history of Mars.

The geologic history of Mars

We distinguish 3 mains eras in the geological history of Mars: the Noachian, the Hesperian, and the Amazonian.

The Noachian probably extended between 4.6 and 3.7 Gyr ago, i.e. it started when Mars formed. At that time, the atmosphere of Mars was much thicker that it is now, it generated greenhouse effect, and liquid water was stable on the surface. It even probably rained on Mars! During that era, the bombardment in the inner Solar System, including on Mars, was very intense, but anyway less intense than the Late Heavy Bombardment, which happened at the end of the Noachian. Many are tempted to consider it to be the cause of the change of era. Anyway, many terrains of the south hemisphere of Mars, and craters, date from the Noachian. And almost all of the river beds as well.

After the Noachian came the Hesperian, probably between 3.7 and 3.2 Gyr ago. It was a period of intense volcanic activity, during which the bombardment declined, and the atmosphere thinned. Then came the Amazonian, which is still on-going, and which is a much quieter era. The volcanic activity has declined as well.

So, almost all of the valley networks date from the Noachian. Let us now see how they formed.

Use of recent data

We owe to the space missions accurate maps of Mars. From these maps, the authors have studied a limited data set of 63 valley networks, 13 of them with a interior channel, the 50 remaining ones without. The interior channel is the former river bed, while the valley represents the area, which has been sculpted by the river. The absence of interior channel probably means that either they are too narrow to be detectable, or have been eroded.

These valley networks are located on sloppy areas, most of them close to the equator. The authors needed the following information:

  1. area,
  2. eroded volume,
  3. valley slopes,
  4. width and depth of the interior channel.

To get this information, they combined topographic data from the instrument MOLA (for Mars Orbiter Laser Altimeter) on board Mars Global Surveyor (1997-2006) with THEMIS (THermal Emission Imaging System, on board Mars Odyssey, still operating). MOLA permits 3-D imagery, with a vertical resolution of 30 cm/pixel (in other words, the accuracy of the altitude) and a horizontal one of 460 m/pixel, while the THEMIS data used by the authors are 2D-data, with a resolution of 100 m /pixel. When the authors judged necessary, they supplemented these data with CTX data (ConTeXt camera, on board Mars Reconnaissance Orbiter, still ongoing), with a resolution up to 6 m/pixel.

These information are very useful to estimate the formation time and the erosion rate of the valley network.

Dynamics of formation of a river bed

They estimated these quantities from the volume of sediments, which should have been transported to create the valley networks. The idea is, while water is flowing, assisted by the Martian surface gravity (fortunately, this number is very well known, and is roughly one-third of the gravity on Earth) and by the slope, it transports material. The authors assumed in their calculations that this material was only sediments, i.e. they neglected rock transport, and they did the maths.

Several competing models exist for sediment transport. This is actually difficult to constrain, given the uncertainties on the sediments themselves. Such phenomena also exist on Earth, but the numbers are very different for instance if you are in Iceland or in the Atacama Desert.

It also depends on the intermittence: is the water flow constant? You can say yes to make your life easier, but is it true? On Earth, you have seasonal variations… why not on Mars? A constant water flow means an intermittence of 100%, while no water means 0%.

And keep also in mind that the water flow depends on the atmospheric conditions: is the air wet or pretty arid? We can answer this question for the present atmospheric conditions, but how was it in the Noachian?

No icy Noachian

And this is one result of the present study: there must have been some evaporation in the Noachian, which means that it was not cold and icy. The authors show that such a Noachian would be inconsistent with the valley networks, as we presently observe them.

However, they get large uncertainties on the formation timescales of the valley networks, i.e. between 500 years and almost twice the age of the Solar System. They have anyway median numbers, i.e.

  • 30 kyr for a continuous sediment flow,
  • 500 kyr with an intermittence of 5%,
  • 3 Myr with an intermittence of 1%,
  • 30 Myr with an intermittence of 0.1%.

And from the data, they estimate that the intermittence should be in the range 1%-5%, which corresponds humid (5%) and semiarid/arid environments. This is how they can rule out the cold and icy Noachian.

The study and its authors

And that’s it for today! Please do not forget to comment. You can also subscribe to the RSS feed, and follow me on Twitter, Facebook, Instagram, and Pinterest.

Saturn sends us meteorites

Hi there! First I would like to thank you for following me on Facebook. The Planetary Mechanics page has reached 1,000 followers!

OK, now back to business. Did you know that our Earth is intensively bombarded from space? You have recently heard of this Chinese space station, Tiangong-1… in that case, it was man-made stuff. But we are intensively bombarded by natural space material. Most of it is so small that it is destroyed when entering the atmosphere, but sometimes it arrives to us as stones… And in extreme cases, the impactor is so large that its impact may generate an extinction event. The Chicxulub crater, in Mexico, is thought to result from the impact, which aftermath provoked the extinction of the dinosaurs, some 66 Myr ago.

The meteorites I speak about today are the ones, which fall on the Earth every year. This is the opportunity to discuss about Identification of meteorite source regions in the Solar System, which has recently been accepted for publication in Icarus. In that study, the authors determine the origin of 25 meteorites, from their observed trajectories just before they hit us.

Meteorites bombard the Earth

We estimate that currently 60 tons of cosmic material fall on the Earth every day. This seems huge, but actually most of it arrives to us as dust, since the original object does not survive its entry into the atmosphere. In fact, the larger the meteorite, the less frequent it falls on us. 4-m objects arrive every ~16 months, 10-m ones every ~10 years, and 100-m ones every ~5,200 years. And they arrive somewhere on Earth… do not forget that most of the surface of our planet is water. So, don’t worry.

The contact of such a small object with the atmosphere may generate an airburst, which itself could be detected, in many frequencies. I mean, you may hear it, you may see it (make a wish), it can also disturb the radio emissions. This motivated the existence of several observation programs, dedicated to the detection of meteors.

Observation networks

Programs of observation exist at least since 1959, originally under the impulse of Ondřejov Observatory (Czech Republic). These are usually national programs, e.g.

and there are probably more. These are networks of camera, which systematically record the sky, accumulating data which are then automatically treated to detect meteors. The detection of a meteors from different location permit to determine its trajectory.

Detection of a fireball by FRIPON, in September 2016. © FRIPON
Detection of a fireball by FRIPON, in September 2016. © FRIPON

Identifying the source

As I said, multiple detections, at different locations, of a fireball, permit to derive its trajectory. This trajectory gives in particular the radiant, which is the direction from which the meteorite, or the impactor, seems to come. The authors are also interested in the velocity of the object.

The velocity and the radiant are determined with respect to the Earth. Once they are determined, the authors translated them into heliocentric elements, i.e. they determined the pre-impact trajectory of the object with respect to the Sun. And this makes sense, since Solar System objects orbit the Sun! This trajectory is made of orbital elements, i.e. semimajor axis, eccentricity, inclination, and the uncertainties associated. Don’t forget that the observations have an accuracy, which you must consider when you use the data. The magnitude of the fireball tells us something on the size of the impactor as well.

From these data, the authors wondered from where the object should come from.

7 candidates as reservoirs of meteorites

The authors identified 7 possible sources for these impactors. These regions are the densest parts of the Main Asteroid Belt.
These are:

  1. the Hungaria family. These asteroids have a semimajor axis between 1.78 and 2 astronomical units, and an inclination between 16° and 34° with respect to the ecliptic, i.e. the orbit of the Earth,
  2. the ν6 resonance: these are bodies, which eccentricity raise because excited by Saturn. They orbit at a location, where they are sensitive to the precessional motion of the pericentre of Saturn. The raise of their eccentricity make these bodies unstable, and good candidates for Earth-crossers. Their semimajor axis is slightly smaller than 2 AU.
  3. the Phocaea family: this is a collisional family of stony asteroids. Their semimajor axes lie between 2.25 and 2.5 AU, their eccentricities are larger than 0.1, and their inclinations are between 18° and 32°. They are known to be a source of Mars-crossers.
  4. the 3:1 MMR (mean-motion resonance with Jupiter): these bodies perform exactly 3 orbits around the Sun while Jupiter makes one. They lie at 2.5 AU. The perturbation by Jupiter tends to empty this zone, which is called a Kirkwood gap.
  5. the 5:2 MMR, at 2.82 AU. This is another Kirkwood gap.
  6. the 2:1 MMR, at 3.27 AU, also known as Hecuba gap,
  7. the Jupiter Family Comets. These are comets, which orbital periods around the Sun are shorter than 20 years, and which inclinations are smaller than 30° with respect to the ecliptic. They are likely to be significantly perturbed by Jupiter.

For each of the 25 referenced meteorites, the authors computed the probability of each of these regions to be the source, in considering the orbital elements (semimajor axis, eccentricity, and inclination) and the magnitude of the object. Indeed, the magnitude is correlated with the size, which is itself correlated with the material constituting it. The reason is that these Earth-crossers orbit the Sun on eccentric orbits, and at their pericentre, i.e. the closest approach to the Sun, they experience tides, which threaten their very existence. In other words, they might be disrupted. Particularly, a large body made of weak material cannot survive.

And now, the results!

Saturn send meteorites to the Earth!

The authors find that the most probable source for the meteorites is the ν6 secular resonance, i.e. with Saturn. In other words, Saturn sends meteorites to the Earth! Beside this, the Hungaria family and the 3:1 mean-motion resonance with Jupiter are probable sources as well. On the contrary, you can forget the Phocaea family and the 2:1 MMR as possible sources.
It appears that the inner belt is more likely to be the source of meteorites than the outer one. Actually, the outer belt mostly contains carbonaceous asteroids, which produce weak meteoroids.

The authors honestly recall that previous studies found similar results. Theirs also contains an analysis of the influence of the uncertainty on the trajectories, and of the impact velocity with the Earth. This influence appears to be pretty marginal.

Anyway, the future will benefit from more data, i.e. more detections and trajectory recoveries. So, additional results are to be expected, just be patient!

The study and its authors

  • You can find the study here, on the website of Icarus. This study is in open access, which means that the authors paid extra fees to make the study available to us. Many thanks to them!
  • You can visit here the website of Mikael Granvik, the first author of the study,
  • and the one of the second author, Peter Brown.

And that’s it for today! Please do not forget to comment. You can also subscribe to the RSS feed, and follow me on Twitter, Facebook, Instagram, and Pinterest.