[meteorite-list] Meteorite-list Digest, Vol 163, Issue 22

From: jack satkoski <jackoski_at_meteoritecentral.com>
Date: Mon, 19 Sep 2016 17:33:40 +0000 (UTC)
Message-ID: <1132583287.1097624.1474306421010_at_mail.yahoo.com>

Subject: petrographic studies of meteorites

Would like to establish connections with those interested in the petrographic side of meteorite classification. jackoski at yahoo.com
Jack Satkoski



On Sunday, September 18, 2016 10:27 PM, "meteorite-list-request at meteoritecentral.com" <meteorite-list-request at meteoritecentral.com> wrote:



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Today's Topics:

   1. Meteorite Picture of the Day (valparint at aol.com)
   2. Test for Damp Ground at Mars' Seasonal Streaks Finds None
      (Ron Baalke)
   3. NASA Awards Launch Services Contract for Mars 2020 Rover
      Mission (Ron Baalke)
   4. Dawn Sets Course for Higher Orbit (Ron Baalke)
   5. Ceres' Geological Activity, Ice Revealed in New Research
      (Ron Baalke)
   6. NASA Approves 2018 Launch of Mars InSight Mission (Ron Baalke)


----------------------------------------------------------------------

Message: 1
Date: Sun, 18 Sep 2016 00:00:11 -0700
From: <valparint at aol.com>
To: <meteorite-list at meteoritecentral.com>
Subject: [meteorite-list] Meteorite Picture of the Day
Message-ID: <1C3FABCA3ADB423882B09A15756AB8E7 at Seuthopolis>
Content-Type: text/plain

Today's Meteorite Picture of the Day: Bassikounou

Contributed by: Rob Lenssen

http://www.tucsonmeteorites.com/mpodmain.asp?DD=09/18/2016


------------------------------

Message: 2
Date: Sun, 18 Sep 2016 20:37:32 -0700 (PDT)
From: Ron Baalke <baalke at zagami.jpl.nasa.gov>
To: meteorite-list at meteoritecentral.com (Meteorite Mailing List)
Subject: [meteorite-list] Test for Damp Ground at Mars' Seasonal
    Streaks Finds None
Message-ID: <201609190337.u8J3bWVD015173 at zagami.jpl.nasa.gov>
Content-Type: text/plain; charset=us-ascii


http://www.jpl.nasa.gov/news/news.php?feature=6597

Test for Damp Ground at Mars' Seasonal Streaks Finds None
Jet Propulsion Laboratory
August 23, 2016

Seasonal dark streaks on Mars that have become one of the hottest topics
in interplanetary research don't hold much water, according to the latest
findings from a NASA spacecraft orbiting Mars.

The new results from NASA's Mars Odyssey mission rely on ground temperature,
measured by infrared imaging using the spacecraft's Thermal Emission Imaging
System (THEMIS). They do not contradict last year's identification of
hydrated salt at these flows, which since their 2011 discovery have been
regarded as possible markers for the presence of liquid water on modern
Mars. However, the temperature measurements now identify an upper limit
on how much water is present at these darkened streaks: about as much
as in the driest desert sands on Earth.

When water is present in the spaces between particles of soil or grains
of sand, it affects how quickly a patch of ground heats up during the
day and cools off at night.

"We used a very sensitive technique to quantify the amount of water associated
with these features," said Christopher Edwards of Northern Arizona University,
Flagstaff. "The results are consistent with no moisture at all and set
an upper limit at three percent water."

The features, called recurring slope lineae or RSL, have been identified
at dozens of sites on Mars. A darkening of the ground extends downhill
in fingerlike flows during spring or summer, fades away in fall and winter,
then repeats the pattern in another year at the same location. The process
that causes the streaks to appear is still a puzzle.

"Some type of water-related activity at the uphill end still might be
a factor in triggering RSL, but the darkness of the ground is not associated
with large amounts of water, either liquid or frozen," Edwards said. "Totally
dry mechanisms for explaining RSL should not be ruled out."

He and Sylvain Piqueux of NASA's Jet Propulsion Laboratory, Pasadena,
California, analyzed several years of THEMIS infrared observations of
a crater-wall region within the large Valles Marineris canyon system on
Mars. Numerous RSL features sit close together in some parts of the study
region. Edwards and Piqueux compared nighttime temperatures of patches
of ground averaging about 44 percent RSL features, in the area, to temperatures
of nearby slopes with no RSL. They found no detectable difference, even
during seasons when RSL were actively growing.

The report of these findings by Edwards and Piqueux has been accepted
by the peer-reviewed Geophysical Research Letters and is available online.

There is some margin of error in assessing ground temperatures with the
multiple THEMIS observations used in this study, enough to leave the possibility
that the RSL sites differed undetectably from non-RSL sites by as much
as 1.8 degrees Fahrenheit (1 Celsius degree). The researchers used that
largest possible difference to calculate the maximum possible amount of
water -- either liquid or frozen -- in the surface material.

How deeply moisture reaches beneath the surface, as well as the amount
of water present right at the surface, affects how quickly the surface
loses heat. The new study calculates that if RSL have only a wafer-thin
layer of water-containing soil, that layer contains no more than about
an ounce of water per two pounds of soil (30 grams water per kilogram
of soil). That is about the same concentration of water as in the surface
material of the Atacama Desert and Antarctic Dry Valleys, the driest places
on Earth. If the water-containing layer at RSL is thicker, the amount
of water per pound or kilogram of soil would need to be even less, to
stay consistent with the temperature measurements.

Research published last year identified hydrated salts in the surface
composition of RSL sites, with an increase during the season when streaks
are active. Hydrated salts hold water molecules affecting the crystalline
structure of the salt.

"Our findings are consistent with the presence of hydrated salts, because
you can have hydrated salt without having enough for the water to start
filling pore spaces between particles," Edwards said. "Salts can become
hydrated by pulling water vapor from the atmosphere, with no need for
an underground source of the water."

"Through additional data and studies, we are learning more about these
puzzling seasonal features -- narrowing the range of possible explanations,"
said Michael Meyer. "It just shows us that we still have much to learn
about Mars and its potential as a habitat for life."

The new study touches on additional factors that add to understanding
of RSL.

-- If RSL were seasonal flows of briny water followed by evaporation,
annual buildup of crust-forming salt should affect temperature properties.
So the lack of a temperature difference between RSL and non-RSL sites
is evidence against evaporating brines.

-- Lack of a temperature difference is also evidence against RSL being
cascades of dry material with different thermal properties than the pre-existing
slope material, such as would be the case with annual avalanching of powdery
dust that accumulates from dusty air.

Arizona State University, Tempe, provided and operates the THEMIS camera,
which records observations in both infrared and visible-light wavelengths.
JPL, a division of Caltech, manages the Mars Odyssey project for NASA.
Lockheed Martin Space Systems, Denver, built the orbiter and collaborates
with JPL to operate it.

Updated (Aug. 26 at 11:00 a.m.) to correct the conversion to 30 grams
of water per kilogram of soil as the upper limit on amount of water in
the soil.

News Media Contact
Guy Webster
Jet Propulsion Laboratory, Pasadena, Calif.
818-354-6278
guy.webster at jpl.nasa.gov

Dwayne Brown / Laurie Cantillo
NASA Headquarters, Washington
202-358-1726 / 202-358-1077
dwayne.c.brown at nasa.gov / laura.l.cantillo at nasa.gov

2016-215



------------------------------

Message: 3
Date: Sun, 18 Sep 2016 20:38:52 -0700 (PDT)
From: Ron Baalke <baalke at zagami.jpl.nasa.gov>
To: meteorite-list at meteoritecentral.com (Meteorite Mailing List)
Subject: [meteorite-list] NASA Awards Launch Services Contract for
    Mars 2020 Rover Mission
Message-ID: <201609190338.u8J3cqaN016170 at zagami.jpl.nasa.gov>
Content-Type: text/plain; charset=us-ascii


http://www.jpl.nasa.gov/news/news.php?feature=6603

NASA Awards Launch Services Contract for Mars 2020 Rover Mission
Jet Propulsion Laboratory
August 25, 2016

NASA has selected United Launch Services LLC of Centennial, Colorado,
to provide launch services for a mission that will address high-priority
science goals for the agency's Journey to Mars.

Mars 2020 is targeted for launch in July 2020 aboard an Atlas V 541 rocket
from Space Launch Complex 41 at Cape Canaveral Air Force Station in Florida.
The rover will conduct geological assessments of its landing site on Mars,
determine the habitability of the environment, search for signs of ancient
Martian life, and assess natural resources and hazards for future human
explorers.

Additionally, scientists will use the instruments aboard the rover to
identify and collect samples of rock and soil, encase them in sealed tubes,
and leave them on the surface of Mars for potential return to Earth by
a future mission to the Red Planet.

The mission will build on the achievements of Curiosity and other Mars
Exploration Program missions, and offer opportunities to deploy new capabilities
developed through investments by NASA's Space Technology Program and Human
Exploration and Operations Mission Directorate, as well as contributions
from international partners.

The Mars 2020 rover mission presents new opportunities to learn how future
human explorers could use natural resources available on the surface of
the Red Planet. An ability to live off the land could reduce costs and
engineering challenges posed by Mars exploration.

The total cost for NASA to launch Mars 2020 is approximately $243 million,
which includes: the launch service; spacecraft and spacecraft power source
processing; planetary protection processing; launch vehicle integration;
and tracking, data and telemetry support.

NASA is on an ambitious journey to Mars that includes sending humans to
the Red Planet. The robotic missions of NASA's Planetary Science Division
are leading the way with the upcoming Mars 2020 rover, the InSight lander
mission targeted for 2018, Opportunity and Curiosity rovers currently
exploring the Martian surface, Odyssey and Mars Reconnaissance Orbiter
spacecraft currently orbiting the planet, and the Mars Atmosphere and
Volatile Evolution Mission (MAVEN) orbiter, which is helping scientists
understand what happened to the planet's atmosphere.

NASA's Launch Services Program at Kennedy Space Center in Florida will
manage and oversee the Atlas V launch service for Mars 2020. The Mars
2020 Project at NASA's Jet Propulsion Laboratory in Pasadena, California,
manages the Mars 2020 spacecraft development for the Science Mission Directorate
at NASA Headquarters in Washington.

For more information about NASA's Mars 2020 rover, visit:

http://mars.nasa.gov/mars2020/

For more information about NASA's Launch Services Program, visit:

http://www.nasa.gov/launchservices

News Media Contact
Tabatha Thompson
Headquarters, Washington
202-358-4811
tabatha.t.thompson at nasa.gov

George H. Diller
Kennedy Space Center, Fla.
321-867-2468
george.h.diller at nasa.gov

2016-220



------------------------------

Message: 4
Date: Sun, 18 Sep 2016 20:43:17 -0700 (PDT)
From: Ron Baalke <baalke at zagami.jpl.nasa.gov>
To: meteorite-list at meteoritecentral.com (Meteorite Mailing List)
Subject: [meteorite-list] Dawn Sets Course for Higher Orbit
Message-ID: <201609190343.u8J3hHex018298 at zagami.jpl.nasa.gov>
Content-Type: text/plain; charset=us-ascii


http://www.jpl.nasa.gov/news/news.php?feature=6608

Dawn Sets Course for Higher Orbit
Jet Propulsion Laboratory
August 31, 2016

After studying Ceres for more than eight months from its low-altitude
science orbit, NASA's Dawn spacecraft will move higher up for different
views of the dwarf planet.

Dawn has delivered a wealth of images and other data from its current
perch at 240 miles (385 kilometers) above Ceres' surface, which is closer
to the dwarf planet than the International Space Station is to Earth.
Now, the mission team is pivoting to consider science questions that can
be examined from higher up.

After Dawn completed its prime mission on June 30, having surpassed all
of its scientific objectives at Vesta and at Ceres, NASA extended the
mission to perform new studies of Ceres. One of the factors limiting Dawn's
lifetime is the amount of hydrazine, the propellant needed to orient the
spacecraft to observe Ceres and communicate with Earth. By going to a
higher orbit at Ceres, Dawn will use the remaining hydrazine more sparingly,
because it won't have to work as hard to counter Ceres' gravitational
pull.

"Most spacecraft wouldn't be able to change their orbital altitude so
easily. But thanks to Dawn's uniquely capable ion propulsion system, we
can maneuver the ship to get the greatest scientific return from the mission,"
said Marc Rayman, chief engineer and mission director, based at NASA's
Jet Propulsion Laboratory, Pasadena, California.

On Sept. 2, Dawn will begin spiraling upward to about 910 miles (1,460
kilometers) from Ceres. The altitude will be close to where Dawn was a
year ago, but the orientation of the spacecraft's orbit -- specifically,
the angle between the orbit plane and the sun -- will be different this
time, so the spacecraft will have a different view of the surface.

The mission team is continuing to develop the extended mission itinerary
and will submit a full plan to NASA next month.

Dawn's mission is managed by JPL for NASA's Science Mission Directorate
in Washington. Dawn is a project of the directorate's Discovery Program,
managed by NASA's Marshall Space Flight Center in Huntsville, Alabama.
UCLA is responsible for overall Dawn mission science. Orbital ATK Inc.,
in Dulles, Virginia, designed and built the spacecraft. The German Aerospace
Center, Max Planck Institute for Solar System Research, Italian Space
Agency and Italian National Astrophysical Institute are international
partners on the mission team. For a complete list of mission participants,
visit:

http://dawn.jpl.nasa.gov/mission

More information about Dawn is available at the following sites:

http://dawn.jpl.nasa.gov

News Media Contact
Elizabeth Landau
Jet Propulsion Laboratory, Pasadena, Calif.
818-354-6425
elizabeth.landau at jpl.nasa.gov

2016-227



------------------------------

Message: 5
Date: Sun, 18 Sep 2016 20:45:29 -0700 (PDT)
From: Ron Baalke <baalke at zagami.jpl.nasa.gov>
To: meteorite-list at meteoritecentral.com (Meteorite Mailing List)
Subject: [meteorite-list] Ceres' Geological Activity, Ice Revealed in
    New Research
Message-ID: <201609190345.u8J3jToG019172 at zagami.jpl.nasa.gov>
Content-Type: text/plain; charset=iso-8859-1


http://www.jpl.nasa.gov/news/news.php?feature=6611

Ceres' Geological Activity, Ice Revealed in New Research
Jet Propulsion Laboratory
September 1, 2016

A lonely 3-mile-high (5-kilometer-high) mountain on Ceres is likely volcanic
in origin, and the dwarf planet may have a weak, temporary atmosphere.
These are just two of many new insights about Ceres from NASA's Dawn mission
published this week in six papers in the journal Science.

"Dawn has revealed that Ceres is a diverse world that clearly had geological
activity in its recent past," said Chris Russell, principal investigator
of the Dawn mission, based at the University of California, Los Angeles.

A Temporary Atmosphere

A surprising finding emerged in the paper led by Russell: Dawn may have
detected a weak, temporary atmosphere. Dawn's gamma ray and neutron (GRaND)
detector observed evidence that Ceres had accelerated electrons from the
solar wind to very high energies over a period of about six days. In theory,
the interaction between the solar wind's energetic particles and atmospheric
molecules could explain the GRaND observations.

A temporary atmosphere would be consistent with the water vapor the Herschel
Space Observatory detected at Ceres in 2012-2013. The electrons that GRaND
detected could have been produced by the solar wind hitting the water
molecules that Herschel observed, but scientists are also looking into
alternative explanations.

"We're very excited to follow up on this and the other discoveries about
this fascinating world," Russell said.

Ahuna Mons as a Cryovolcano

Ahuna Mons is a volcanic dome unlike any seen elsewhere in the solar system,
according to a new analysis led by Ottaviano Ruesch of NASA's Goddard
Space Flight Center, Greenbelt, Maryland, and the Universities Space Research
Association. Ruesch and colleagues studied formation models of volcanic
domes, 3-D terrain maps and images from Dawn, as well as analogous geological
features elsewhere in our solar system. This led to the conclusion that
the lonely mountain is likely volcanic in nature. Specifically, it would
be a cryovolcano -- a volcano that erupts a liquid made of volatiles such
as water, instead of silicates. "This is the only known example of a cryovolcano
that potentially formed from a salty mud mix, and that formed in the geologically
recent past," Ruesch said.

For more details on this study, see:
http://www.nasa.gov/feature/goddard/2016/ceres-cryo-volcano

Ceres: Between a Rocky and Icy Place

While Ahuna Mons may have erupted liquid water in the past, Dawn has detected
water in the present, as described in a study led by Jean-Philippe Combe
of the Bear Fight Institute, Winthrop, Washington. Combe and colleagues
used Dawn's visible and infrared mapping spectrometer (VIR) to detect
probable water ice at Oxo Crater, a small, bright, sloped depression at
mid-latitudes on Ceres.

Exposed water-ice is rare on Ceres, but the low density of Ceres, the
impact-generated flows and the very existence of Ahuna Mons suggest that
Ceres' crust does contain a significant component of water-ice. This is
consistent with a study of Ceres' diverse geological features led by Harald
Hiesinger of the Westf?lische Wilhelms-Universit?t, M?nster, Germany.
The diversity of geological features on Ceres is further explored in a
study led by Debra Buczkowski of the Johns Hopkins Applied Physics Laboratory,
Laurel, Maryland.

Impact craters are clearly the most abundant geological feature on Ceres,
and their different shapes help tell the intricate story of Ceres' past.
Craters that are roughly polygonal -- that is, shapes bounded by straight
lines -- hint that Ceres' crust is heavily fractured. In addition, several
Cerean craters have patterns of visible fractures on their floors.

Some, like tiny Oxo, have terraces, while others, such as the large Urvara
Crater (106 miles, 170 kilometers wide), have central peaks. There are
craters with flow-like features, and craters that imprint on other craters,
as well as chains of small craters. Bright areas are peppered across Ceres,
with the most reflective ones in Occator Crater. Some crater shapes could
indicate water-ice in the subsurface.

The dwarf planet's various crater forms are consistent with an outer shell
for Ceres that is not purely ice or rock, but rather a mixture of both
-- a conclusion reflected in other analyses. Scientists also calculated
the ratio of various craters' depths to diameters, and found that some
amount of crater relaxation must have occurred. Additionally, there are
more craters in the northern hemisphere of Ceres than the south, where
the large Urvara and Yalode craters are the dominant features.

"The uneven distribution of craters indicates that the crust is not uniform,
and that Ceres has gone through a complex geological evolution," Hiesinger
said.

Distribution of Surface Materials

What are the rocky materials in Ceres' crust? A study led by Eleonora
Ammannito of the University of California, Los Angeles, finds that clay-forming
minerals called phyllosilicates are all over Ceres. These phyllosilicates
are rich in magnesium and also have some ammonium embedded in their crystalline
structure. Their distribution throughout the dwarf planet's crust indicates
Ceres' surface material has been altered by a global process involving
water.

Although Ceres' phyllosilicates are uniform in their composition, there
are marked differences in how abundant these materials are on the surface.
For example, phyllosilicates are especially prevalent in the region around
the smooth, "pancake"-like crater Kerwan (174 miles, 280 kilometers in
diameter), and less so at Yalode Crater (162 miles, 260 kilometers in
diameter), which has areas of both smooth and rugged terrain around it.
Since Kerwan and Yalode are similar in size, this may mean that the composition
of the material into which they impacted may be different. Craters Dantu
and Haulani both formed recently in geologic time, but also seem to differ
in composition.

"In comparing craters such as Dantu and Haulani, we find that their different
material mixtures could extend beneath the surface for miles, or even
tens of miles in the case of the larger Dantu," Ammannito said.

Looking Higher

Now in its extended mission, the Dawn spacecraft has delivered a wealth
of images and other data from its current perch at 240 miles (385 kilometers)
above Ceres' surface, which is closer to the dwarf planet than the International
Space Station is to Earth. The spacecraft will be increasing its altitude
at Ceres on Sept. 2, as scientists consider questions that can be examined
from higher up.

Dawn's mission is managed by JPL for NASA's Science Mission Directorate
in Washington. Dawn is a project of the directorate's Discovery Program,
managed by NASA's Marshall Space Flight Center in Huntsville, Alabama.
UCLA is responsible for overall Dawn mission science. Orbital ATK Inc.,
in Dulles, Virginia, designed and built the spacecraft. The German Aerospace
Center, Max Planck Institute for Solar System Research, Italian Space
Agency and Italian National Astrophysical Institute are international
partners on the mission team. For a complete list of mission participants,
visit:

http://dawn.jpl.nasa.gov/mission

More information about Dawn is available at the following sites:

http://dawn.jpl.nasa.gov

http://www.nasa.gov/dawn

News Media Contact
Elizabeth Landau
Jet Propulsion Laboratory, Pasadena, Calif.
818-354-6425
elizabeth.landau at jpl.nasa.gov

2016-229



------------------------------

Message: 6
Date: Sun, 18 Sep 2016 20:47:05 -0700 (PDT)
From: Ron Baalke <baalke at zagami.jpl.nasa.gov>
To: meteorite-list at meteoritecentral.com (Meteorite Mailing List)
Subject: [meteorite-list] NASA Approves 2018 Launch of Mars InSight
    Mission
Message-ID: <201609190347.u8J3l5dm020060 at zagami.jpl.nasa.gov>
Content-Type: text/plain; charset=iso-8859-1


http://www.jpl.nasa.gov/news/news.php?feature=6612

NASA Approves 2018 Launch of Mars InSight Mission
Jet Propulsion Laboratory
September 2, 2016

NASA is moving forward with a spring 2018 launch of its InSight mission
to study the deep interior of Mars, following final approval this week
by the agency's Science Mission Directorate.

The Interior Exploration using Seismic Investigations, Geodesy and Heat
Transport (InSight) mission was originally scheduled to launch in March
of this year, but NASA suspended launch preparations in December due to
a vacuum leak in its prime science instrument, the Seismic Experiment
for Interior Structure (SEIS).

The new launch period for the mission begins May 5, 2018, with a Mars
landing scheduled for Nov. 26, 2018. The next launch opportunity is driven
by orbital dynamics, so 2018 is the soonest the lander can be on its way.

"Our robotic scientific explorers such as InSight are paving the way toward
an ambitious journey to send humans to the Red Planet," said Geoff Yoder,
acting associate administrator for NASA's Science Mission Directorate,
in Washington. "It's gratifying that we are moving forward with this important
mission to help us better understand the origins of Mars and all the rocky
planets, including Earth."

The SEIS instrument -- designed to measure ground movements as small as
half the radius of a hydrogen atom -- requires a perfect vacuum seal around
its three main sensors in order to withstand harsh conditions on the Red
Planet. Under what's known as the mission "replan," NASA's Jet Propulsion
Laboratory in Pasadena, California, will be responsible for redesigning,
developing and qualifying the instrument's evacuated container and the
electrical feedthroughs that failed previously. France's space agency,
the Centre National d'?tudes Spatiales (CNES), will focus on developing
and delivering the key sensors for SEIS, integration of the sensors into
the container, and the final integration of the instrument onto the spacecraft.

The German Aerospace Center (DLR) is contributing the Heat Flow and Physical
Properties Package (HP3) to InSight's science payload.

NASA's budget for InSight was $675 million. The instrument redesign and
two-year delay add $153.8 million. The additional cost will not delay
or cancel any current missions, though there may be fewer opportunities
for new missions in future years, from fiscal years 2017-2020.

InSight's primary goal is to help us understand how rocky planets formed
and evolved. Jim Green, director of NASA's Planetary Science Division,
said, "We've concluded that a replanned InSight mission for launch in
2018 is the best approach to fulfill these long-sought, high-priority
science objectives."

CNES President Jean-Yves Le Gall added, "This confirmation of the launch
plan for InSight is excellent news and an unparalleled opportunity to
learn more about the internal structure of the Red Planet, which is currently
of major interest to the international science community."

The InSight Project is managed by JPL for NASA's Science Mission Directorate,
Washington. Lockheed Martin Space Systems, Denver, built the spacecraft.
InSight is part of NASA's Discovery Program, which is managed by NASA's
Marshall Space Flight Center in Huntsville, Alabama.

News Media Contact
Guy Webster
Jet Propulsion Laboratory, Pasadena, Calif.
818-354-6278
guy.webster at jpl.nasa.gov

Dwayne Brown / Laurie Cantillo
NASA Headquarters, Washington
202-358-1726 / 202-358-1077
dwayne.c.brown at nasa.gov / laura.l.cantillo at nasa.gov


------------------------------

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End of Meteorite-list Digest, Vol 163, Issue 22
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Received on Mon 19 Sep 2016 01:33:40 PM PDT