Дата: 02 декабря 1998 (1998-12-02)
От: Alexander Bondugin
Тема: Готовится к старту первый американский элемент МКС
Привет всем!
Вот, свалилось из Internet...
Готовится к старту первый американский элемент Международной
космической станции
[NASA] Запуск первого американского элемента Международной
космической станции намечен на 3 декабря. Это будет стыковочный
модуль Unity (в интерпретации Российского космического агентства -
Node1). Этот элемент будет пристыкован к уже находящемуся на орбите
модулю "Заря" 6 декабря экипажем космического корабля Space Shuttle
Endeavour.
Модуль Unity (на снимке)
построен компанией Boeing в
Центре космических полетов им.
Маршалла в Хантсвилле (шт.
Алабама). Он имеет
шестигранную боковую
поверхность. К нему будут
пристыковываться все следующие
американские модули станции.
Чтобы облегчить "ношу"
корабля Endeavour на "шаттл" будет установлен новый сверхлегкий
внешний бак с горючим. Первое успешное испытание этого бака
состоялось в июне 1998 г. Его размеры такие же как у старого бака, но
весит он на 3,4 тонны меньше, что весьма существенно при запуске
тяжелых элементов космической станции.
Источник: InfoArt News Agency
Hа сегодня все, пока!
=SANA=
Дата: 02 декабря 1998 (1998-12-02)
От: Alexander Bondugin
Тема: Готовится к старту первый американский элемент МКС (картинка) [1/3]
Привет всем!
Вот, свалилось из Internet...
section 1 of 3 of file unity3_m.jpg < uuencode 5.32 by R.E.M. >
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sum -r/size 25682/12423 section (from "begin" to last encoded line)
Hа сегодня все, пока!
=SANA=
Дата: 02 декабря 1998 (1998-12-02)
От: Alexander Bondugin
Тема: Готовится к старту первый американский элемент МКС (картинка) [2/3]
Привет всем!
Вот, свалилось из Internet...
section 2 of 3 of file unity3_m.jpg < uuencode 5.32 by R.E.M. >
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MA2W15@:Y8[L\@-M7<#@A<*X`;')`ZV$\:6?VW[')HFNQ707=Y$\$<#GC/'F.
MH-/N?&MY#(([/0T8DS^8I6"+:U+OA7P$MI=F\O)/M5ZQ8"X$
M7ELB$_<5K%\(6%Y#JFL7MSOCCFE5((C*64*,DL!D@9SC&`>.:U
MM?3?I%PB\'8#Q[$?X4WP_/)/#=-);2PA;AD0R;?WBC&'&">#VS@^PJ?4P&L;
M@>L+_P`JN*LBSPOQ0!'K8(K:[\[3KE;NQ\QДата: 02 декабря 1998 (1998-12-02)
От: Alexander Bondugin
Тема: Готовится к старту первый американский элемент МКС (картинка) [3/3]
Привет всем!
Вот, свалилось из Internet...
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MD&3O.>OKUK1.QCRFO(\<;)<2S3W`>%B`NXKD9X(_AQ4UKJ,,J&R2)3&3:4`^0"-CSD$@UGW,DCQI>Q3.H,K2-'$HVQD$XX^@K.665;61!(VV.10B
MDY"C/8=JKJ[)97"JQ`+`_ETI!RD]N#=19S*[9*%BN`"3G/UI$=7N)(TEV@(<
ML@VY.<#-2W$CM;666(W7$F=O&>0.U0:K_HVJ216X$<YQ.J`L#@#'XU4=V:=Y9N)!U#&*-X$W+GYA0,I,WF,69B`H
MP`3VIR;E"XYQ^2__`%Z6Z51,X`P`.*)B1(ZCA3MR!TH`:'^4Y)!SU'>D)8(%
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M[`"GV_S!RWO_`"H`:@17)+*$)*X=Дата: 02 декабря 1998 (1998-12-02)
От: Alexander Bondugin
Тема: Cameras Aid San Francisco Airport Weather Reports
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Michael Braukus
Headquarters, Washington, DC December 1, 1998
(Phone: 202/358-1979)
Michael Mewhinney
Ames Research Center, Moffett Field, CA
(Phone: 650/604-3937)
Les Dorr
FAA Headquarters, Washington, DC
(Phone: 202/267-3461)
Stephanie Kenitzer
National Weather Service
(Phone: 301/763-8000 ext. 7007)
RELEASE: 98-218
CAMERAS AID SAN FRANCISCO AIRPORT WEATHER REPORTS
New digital video cameras installed by NASA at the San
Carlos, CA, airport control tower, are helping to better report
current weather conditions for aircraft landing at San Francisco
International Airport, some 10 miles away.
Installed by engineers from NASA's Ames Research Center,
Moffett Field, CA, the Airport Approach Zone Camera System enables
air traffic controllers and weather forecasters to track real-time
onset and dissipation of fog and low clouds in the airport's
approach zone, particularly during the late morning. Since many
aircraft arrive at that time, the precise timing of the improved
visibility will improve the airport's ability to operate at or
close to full capacity.
"The big problem with arrivals at San Francisco International
Airport is that the runways are only 750 feet apart; when you
can't use both runways at the same time, you can only land 30
aircraft an hour," said Yuri Gawdiak, an Ames aerospace engineer
and the project leader. San Francisco International Airport is
one of the nation's busiest, with 600-700 landings on a typical
day. With both runways operating simultaneously, 60 aircraft an
hour can land.
"The live pictures allow us to better serve the needs of the
Federal Aviation Administration's (FAA) Air Traffic Management
Specialists, here at the Oakland Air Route Traffic Control Center
in Fremont, CA; the Oakland Bay TRACON (Terminal Radar Approach
Control Facility) at the Oakland International Airport; and at the
Air Traffic Control System Command Center in Washington, DC," said
Walt Strach, National Weather Service Meteorologist in Charge of
the Fremont facility.
The Airport Approach Zone Camera System will significantly
reduce telephone calls between the FAA Oakland Center
meteorologist and the San Francisco Air Traffic Control Tower.
"This should translate into more efficient procedures for flow
control when weather is a factor in landing aircraft at San
Francisco International Airport," Strach said.
"The Airport Approach Zone Camera System is allowing
meteorologists, both in my office and at the National Weather
Service Forecast Office in Monterey, CA, to better see and
understand the local effects of wind currents, and terrain, ocean
and bay influences on the formation and dissipation of clouds and
fog in and around San Francisco International Airport," Strach
said. The Monterey weather office issues aviation, public and
marine forecasts for the entire San Francisco Bay Area.
The high-speed video cameras operate 24 hours-a-day and
provide a 220-degree field of view with rotation, zoom and tilt
capabilities. The cameras are remotely controlled by personnel at
the National Oceanic and Atmospheric Administration (NOAA) weather
center located at the Oakland Air Route Traffic Control Center and
are accessible via a secure web site. Ames engineers will install
similar cameras at the San Francisco International Airport control
tower in the near future.
The Airport Approach Zone Camera System is a joint effort
between Ames, the FAA and NOAA. The project is managed by the
aviation safety monitoring office at Ames and funded by NASA's
aviation safety program.
- end -
Hа сегодня все, пока!
=SANA=
Дата: 02 декабря 1998 (1998-12-02)
От: Alexander Bondugin
Тема: Первый полет американцев на строительство МКС
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Первый полет американцев на строительство Международной
космической станции
[NASA] 3 декабря - официальная дата старта миссии NASA STS-88
на космическом корабле Space Shuttle Endeavour. Это первый вылет
"шаттла" на строительство Международной космической станции. Hа
Endeavour полетит экипаж из 6 человек, кроме того Endeavour повезет в
космос американский модуль Unity, который станет вторым элементом
станции. Его пристыковку к "Заре" и осуществит экипаж.
Запуск Endeavour планируется произвести 3 декабря в 3 ч 59 мин
EST (11 ч 59 мин по московскому времени), но точный момент старта
будет определен за час до указанного времени в соответствии с
измерениями точного положения на орбите модуля "Заря". Экспедиция
продлится 11 дней 19 часов и 49 минут и завершится она 14 декабря в 11
ч 48 мин EST.
Экипаж миссии STS-88: командир Роберт Кабана (Robert Cabana),
штурман Фредрик Старкоу (Fredrick Sturckow), специалисты Hэнси Карри
(Nancy Currie), российский космонавт Сергей Крикалев, Джерри Росс
(Jerry Ross) и Джеймс Hьюмен (James Newman).
Источник: InfoArt News Agency
Hа сегодня все, пока!
=SANA=
Дата: 02 декабря 1998 (1998-12-02)
От: Alexander Bondugin
Тема: Молодые звезды испускают сверхзвуковые потоки газа и пыли
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Молодые звезды испускают сверхзвуковые потоки газа и пыли
[SpaceViews] Астрономы из университета Колорадо получили
доказательства того, что молодые звезды испускают сверхзвуковые
потоки газа и пыли. Их скорость может достигать 500 км/с, а длина -
миллиарды километров. Именно таким образом близлежащие более
массивные звезды "раздевают" небольшие молодые звезды. Сейчас такое
явление имеет место в туманности Ориона - кокон газа и пыли,
окружающий расположенные там звезды, был "содран" ультрафиолетовым
излучением более массивных соседних звезд.
Такие наблюдения могут пролить свет на образование планетных
систем, каковой является и наша Солнечная система. Возможно, Солнце
когда-то было такой "новорожденной" звездой, а из улетевших с ее
поверхности газа и пыли образовались планеты, в том числе и наша
Земля.
Источник: InfoArt News Agency
Hа сегодня все, пока!
=SANA=
Дата: 02 декабря 1998 (1998-12-02)
От: Alexander Bondugin
Тема: Погода может помешать старту Endeavour
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Погода может помешать старту Endeavour
[SpaceViews] Облачная погода может помешать старту космического
челнока Endeavour, намеченному на завтра 3 декабря. Главный метеоролог
по проекту "шаттл" Эд Прайслек (Ed Priselac) считает, что вероятность
того, что запуск будет отложен по погодным условиям равна 60%.
Проблемы с погодой - это слабая видимость и сильные дожди в районе
старта и на посадочной полосе в Космическом центре им. Кеннеди,
которая понадобится для приземления Endeavour в случае аварии вскоре
после старта.
Экипаж Endeavour, в составе которого есть и российский космонавт
Сергей Крикалев, прибыл в Центр им. Кенеди из Хьюстона в воскресенье
вечером.
Источник: InfoArt News Agency
Hа сегодня все, пока!
=SANA=
Дата: 02 декабря 1998 (1998-12-02)
От: Alexander Bondugin
Тема: Mars Global Surveyor Aerobraking Update - November 25, 1998
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Mars Global Surveyor Aerobraking Status Report
Wednesday, November 25 (DOY 326/19:00:00 to DOY 329/19:00:00 UTC)
Last Orbit Covered by this Report = 765
Total Phase I Aerobraking orbits accomplished = 180
Total Phase II Aerobraking orbits accomplished = 192
Total Science Phasing orbits accomplished = 290
Apoapsis altitude = 7787 km
Apoapsis altitude decrease since start of aerobraking = 46239 km
Periapsis altitude = 115.3 km
Current Orbit Period = 05:18:12
Orbit Period decrease since start of aerobraking = 39:41:21
Starting Phase II orbit period = 11:38:02
RECENT EVENTS:
The Mars Global Surveyor spacecraft continues successful phase 2 aerobraking
operations with no concerns. The past 13 drag passes have provided about 11
minutes of orbit period reduction. The current period maintains about a 9
minute lead on the baseline. The dynamic pressure 7-orbit running mean is
0.185 N/m2 which is below the 0.23 N/m2 corridor control trigger limit.
There was 1 corridor control maneuver executed on the apoapsis portion of
orbit 764 to raise periapsis and lower the drag force.
Currently, sequence P762 is controlling the S/C activities. It will be
replaced early this evening with P767 which will control activities starting
with orbit 767 through orbit 770. P762 was to be replaced by P766 but
because of a sequence build error, the P766 product could not be built and
verified in time to radiate to the S/C. The decision was made to allow the
first backup orbit from P762 to control activities for orbit 766 and start
the next sequence with orbit 767. Each sequence continues to be built with 5
primary orbits even though, in order to maintain prime shift builds, only
four may be allowed to execute at times. Orbit timing predictions continue
to be very good.
Subsystems continue to report excellent S/C health and performance. The -Y
solar array yoke has shown no change in structural performance. Attitude
knowledge has been maintained throughout the period with excellent star
processing. The power subsystem reports strong performance with 13.8 %
maximum battery discharge depths each orbit. There is now 3.2 minutes of
primary charger margin. The minimum MOLA laser temperature observed this
period was 12.1°C using a 35 minute warming maneuver each orbit. The largest
temperature increase due to aero-heating was 69°C on the -Y solar array,
cell side. The telecommunications subsystem continues solid performance.
The weekly reset meeting was held today to discuss aerobraking progress and
to review sequence parameter changes. The dynamic pressure running mean was
changed to include 7 orbits, up from 6. The MOLA laser warming maneuver was
shortened in duration by 10 minutes to 25 minutes per orbit. The playback
from corridor control maneuvers was delayed an additional 50 minutes
following the maneuver to assure data is received following Earth
occultation. The number of backup orbits was increased from 2 to 3 each
sequence to allow margin in case ground processing problems do not allow
timely sequence uploads.
UPCOMING EVENTS:
Periapsis for Orbit 766 DOY329/22:10:10 UTC Through
Periapsis for Orbit 788 DOY334/17:04:08 UTC
(Note: MST = UTC-7 hours DOY329=11/25)
SPACECRAFT COMMANDING:
There were 11 command files radiated to the S/C during this period. The
total files radiated since launch is now 3000. These commands were sent in
support of the following activities:
Nominal drag pass sequences (P753, P758, P762)
Nominal corridor control maneuver sequences (A764)
Command loss timer resets
Nominal star catalog and ephemeris file updates
Hа сегодня все, пока!
=SANA=
Дата: 02 декабря 1998 (1998-12-02)
От: Alexander Bondugin
Тема: Mars Global Surveyor Aerobraking Update - November 30, 1998
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Mars Global Surveyor Aerobraking Status Report
Monday, November 30 (DOY 329/19:00:00 to DOY 334/19:00:00 UTC)
Last Orbit Covered by this Report = 788
Total Phase I Aerobraking orbits accomplished = 180
Total Phase II Aerobraking orbits accomplished = 215
Total Science Phasing orbits accomplished = 290
Apoapsis altitude = 7215 km
Apoapsis altitude decrease since start of aerobraking = 46811 km
Periapsis altitude = 111.8 km
Current Orbit Period = 04:59:44
Orbit Period decrease since start of aerobraking = 39:59:49
Starting Phase II orbit period = 11:38:02
RECENT EVENTS:
The spacecraft health and performance remains excellent as the orbit period
is now below 5 hours. The orbit period has been reduced by about 19.5
minutes over the past 23 orbits, close to the baseline schedule. The current
period maintains about a 9 minute lead on the baseline. The dynamic pressure
7-orbit running mean is 0.228 N/m2 which is close to the trigger limit of
0.23 N/m2. A periapsis raise maneuver was ordered and will execute on the
apoapsis portion of orbit 789 to lower the drag pass forces. The
orbit-to-orbit dynamic pressure variability has increased over the past 2
weeks. For this period, the lowest drag force of 0.11 N/m2 was experienced
on orbit 773. The high was recorded on the last orbit, 788, registering 0.33
N/m2.
Currently, sequence P785 is controlling the S/C activities. It will be
replaced early tomorrow morning with P791 which will control activities
starting with orbit 791 through orbit 794. P785 was to be replaced by P790
but because of DSN station gaps, navigation data will not be available for
the P790 build. The decision was made to allow the first backup orbit from
P785 to control activities for orbit 790 and start the next sequence with
orbit 791. Early this reporting period, P771 encountered an error and
halted, leaving the current sequence (P767) the responsibility of executing
orbit 771 as backup. The error, execution of a `Send-Two-Word' command in
the same second as another command, has been encountered before. Automated
tools discovered the error, but the warnings were misinterpreted by ground
personal allowing the error to propagate. Once loaded, the error canceled
the sequence early in its startup. A replacement sequence, P772, was
generated and loaded. A timing error of 320 seconds was experienced on the
backup orbit, which is high but within backup orbit tolerances. The S/C
processed a Sun avoidance maneuver following the 771 drag pass which
resulted in over 20 grams of fuel used. An ISA has been initiated to
document the event. Removal of the `Send-Two-Word' from future sequences was
approved by MCR. This fix will be installed on Wednesday.
Subsystems continue to report excellent S/C health and performance. The -Y
solar array yoke has shown no change in structural performance. Attitude
knowledge has been maintained throughout the period with excellent star
processing. The power subsystem reports strong performance with battery
discharge depths ranging from 10.5% to 13.2%. A larger 15.2% DoD was
experienced during the Sun avoidance maneuver on orbit 771. There continues
to be positive re-charge margin each orbit. The minimum MOLA laser
temperature observed this period was 11.2 °C using a 25 minute warming
maneuver each orbit. The largest temperature increase due to aero-heating
was 61°C on the -Y solar array, cell side. The telecommunications subsystem
continues solid performance.
Earth occultations occur each orbit starting just before apoapsis and
lasting about 1 hour. The MOLA warming maneuver is executed within the
occultation period allowing for maximum ground communication time each
orbit.
UPCOMING EVENTS:
Periapsis for Orbit 789 DOY334/20:35:38 UTC Through
Periapsis for Orbit 798 DOY336/16:52:03 UTC
(Note: MST = UTC-7 hours DOY334=11/30)
SPACECRAFT COMMANDING:
There were 10 command files radiated to the S/C during this period. The
total files radiated since launch is now 3010. These commands were sent in
support of the following activities:
Nominal drag pass sequences (P767, P771, P772, P775, P780, P785)
Nominal corridor control maneuver sequences (A789)
Command loss timer resets
Hа сегодня все, пока!
=SANA=
Дата: 02 декабря 1998 (1998-12-02)
От: Alexander Bondugin
Тема: 'Mirage' used to measure age of Universe (Forwarded)
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Commonwealth Scientific and
Industrial Research Organisation
Australia
Ms Rosie Schmedding (02) 6276-6520
Mobile (0418) 622-653
Fax (02) 6276-6821
Media Release: 1 December 1998 Ref 98/280
'MIRAGE' USED TO MEASURE AGE OF UNIVERSE
An international team led by a young Australian scientist has used CSIRO's
Australia Telescope to measure how fast the Universe is expanding -- and
found it to be both older and larger than previously thought.
The expansion is measured as a number called the Hubble Constant. It is used
to calculate how big and how old the Universe is.
The observing team used a new method that avoids the built-in uncertainties
in older methods and found the universe to be 15 billion years old.
Astronomers have been wrangling over the value of the Hubble Constant -- a
number that indicates the expansion rate of the universe and hence its
age -- for several decades. Measuring it is a key problem that the Hubble
Space Telescope was built to solve.
"Our value is about 20% lower than the one got with the Hubble Space Telescope
in 1994," said Dr Jim Lovell, leader of the team that made the measurement.
The Hubble Constant is named after American astronomer Edwin Hubble, who in
the 1920s found that other galaxies were moving away from ours.
"The Universe as a whole is expanding, like a lump of bread dough rising,"
Dr Lovell explained. "Like currants in the dough, the galaxies are all moving
away from each other."
"The further away a galaxy is, the faster it is moving away from us. The
Hubble Constant links the galaxy's distance with its speed."
"Measuring the speed at which a galaxy is receding is fairly easy," said
CSIRO's Dr David Jauncey, another member of the observing team. "But
accurately measuring its distance is very hard."
The usual way to measure a galaxy's distance has been to look for objects
whose intrinsic brightness is known. "The further off these things are, the
fainter they look, and as we know how bright they are intrinsically, we can
calculate their distances," said Dr Jauncey. "The usual objects to use have
been rare, special pulsating stars called Cepheids, or some kinds of
exploding stars (supernovae)."
In 1994 a team used the Hubble Space Telescope to measure the brightnesses
of 20 Cepheids in a galaxy called M100. From these, they calculated its
distance was 56 million light-years and from that they got a figure for the
Hubble Constant.
Dr Lovell used a different, more direct method.
"We have been looking at light from a very distant quasar -- a galaxy with
an extremely bright centre," he said.
"Quasars usually look like small spots but this one looks like a ring. Its
image has been distorted by the gravity of a galaxy lying between us and the
quasar. We're seeing a sort of mirage of the distant quasar," explained Dr
Lovell.
The process that makes the mirage is called gravitational lensing, and was
predicted by Einstein.
Light that ends up in one side of the ring has travelled along a different
path to the light on the other side, he said.
"These paths are different lengths. When the quasar puts out more radiation,
one side of the ring varies before the other. We put that time-lag together
with other information we know about the system -- redshifts and angles --
and out pops the Hubble Constant."
The technique sounds simple but it has taken until now to use it successfully,
says Dr Lovell, because the lens has to meet a number of conditions. "It has
to be strong enough to see clearly, you have to be able to measure the
distances to both the background quasar and the lensing galaxy, and the
quasar has to vary over time in just the right way.
What we've got is one of the good ones -- a so-called 'golden lens', the type
everyone has been looking for," Dr Lovell said.
This 'golden lens' is called PKS1830-211 and was discovered in 1991 by
astronomers from the CSIRO's Australia Telescope National Facility (ATNF),
the University of Tasmania and NASA's Jet Propulsion Laboratory. It is the
strongest gravitational lens ever found, 10 times brighter than any other
known. It is 14 billion light-years away while the galaxy distorting its
image is 8 billion light-years away.
"As more good lens systems become known, more groups are trying to measure
the Hubble Constant in this way," said Dr Lovell.
The twist is that the Hubble Constant is probably not constant at all.
"We think it has varied over the lifetime of the Universe," said Dr Jauncey.
"From other work it seems that the Universe is now expanding faster than it
used to. The value we've measured is for a particular point in the Universe's
history, and will help us to build up a picture of how the rate of expansion
has changed."
More information:
Dr David Jauncey
CSIRO
(02) 6216 7220 (B.H.) email: Dave.Jauncey@atnf.csiro.au
Dr Jim Lovell
Institute of Space and Astronautical Science, Japan
(+81) 427-59-8346 email:jlovell@vsop.isas.ac.jp
More information is also available on the WWW:
General information plus still images:
http://halca.vsop.isas.ac.jp/1830-211/
A short run-down on the Hubble Constant:
http://astroweb.onysd.wednet.edu/sciweb/astronomy/astrophysics/hnought.html
An animation of a gravitational lens prepared by Jim Lovell:
In Australia: http://www-ra.phys.utas.edu.au/~jlovell/simlens
In Japan: http://halca.vsop.isas.ac.jp/~jlovell/simlens
Andrew Yee
ayee@nova.astro.utoronto.ca
Hа сегодня все, пока!
=SANA=
Дата: 02 декабря 1998 (1998-12-02)
От: Alexander Bondugin
Тема: NASA Announces Research Grants In Microgravity Biotechnology
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Renee N. Juhans
Headquarters, Washington, DC December 1, 1998
(Phone: 202/358-1712)
RELEASE: 98-217
NASA ANNOUNCES RESEARCH GRANTS IN MICROGRAVITY BIOTECHNOLOGY
NASA has selected 48 researchers to receive grants totaling
approximately $33 million to conduct microgravity biotechnology
research. Forty of the grants are to conduct ground-based
research, while the remaining eight are flight definition efforts.
Fourteen of these grants are for continuation of work currently
being funded by NASA, but the majority (34) represent new research
efforts.
Sponsored by NASA's Office of Life and Microgravity Science
and Applications, this research allows investigators to take
advantage of a low-gravity environment to improve understanding of
fundamental physical and chemical processes associated with
biotechnology. The research support by NASA under this
announcement includes protein crystallization, cell science
studies, and new technology development. This research may affect
such important areas as structure-based drug design, tissue
engineering, and biosensor development.
The investigators will have NASA's microgravity research
facilities such as aircraft flying parabolic trajectories and
sounding rockets at their disposal; the flight-definition
investigators will work toward experiments on the International
Space Station.
NASA received 165 proposals in response to its announcement
in this research area. These proposals were peer-reviewed by
scientific and technical experts from academia, government and
industry. In addition, those proposals selected for flight
definition were reviewed in terms of engineering feasibility by a
team from NASA's Marshall Space Flight Center. Huntsville, AL.
A list of awardees (by state), their institutions, and
research titles can be found via Internet at:
ftp://ftp.hq.nasa.gov/pub/pao/pressrel/1998/98-217a.txt
-end-
Hа сегодня все, пока!
=SANA=
Дата: 02 декабря 1998 (1998-12-02)
От: Alexander Bondugin
Тема: NASA Selects Litton/PRC For NASA Sounding Rocket Program
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Don Savage
Headquarters, Washington, DC December 1, 1998
(Phone: 202/358-1727)
Keith Koehler
Wallops Flight Facility, Wallops Island, VA
(Phone: 757/824-1579)
RELEASE: C98-t
NASA SELECTS LITTON/PRC FOR NASA SOUNDING ROCKET PROGRAM
NASA has selected Litton/PRC of McLean, VA, to perform
services for a new contract which consolidates several previous
service and supply contracts and other work supporting NASA's
Sounding Rocket Program. The contract begins Feb. 1, 1999.
Services include designing, fabricating, integrating,
testing and performing mission operations for sounding rocket
missions.
"We are confident that the Litton/PRC team will continue
the tradition of successful sounding rocket launches from sites
worldwide in support of space and Earth science communities," said
Mary Kicza, Associate Director of NASA's Goddard Space Flight
Center, Greenbelt, MD.
The work will be performed at Goddard's Wallops Flight
Facility, Wallops Island, VA, and at various off-site locations
worldwide in support of Wallops projects. The services will be
provided under a performance-based, cost-plus award and incentive
fee, indefinite delivery/indefinite quantity (IDIQ) contract.
The basic contract is for four years with two, three-year
options. The contract's minimum IDIQ value for the four-year
basic contract is $11.9 million, and the potential maximum IDIQ
value for the basic contract period is $211.8 million. The
minimum value for the basic and two, three-year option periods is
$31.9 million and the potential maximum value for the basic and
two, three year option periods is $572.5 million.
The contractor also will provide performance task-order
services for various Center programs using NASA Sounding Rocket
Operations Contract government-furnished property, such as the
fabrication and environmental test facilities at NASA's Wallops
Flight Facility.
The NASA Sounding Rocket Operations Contract is an integral
part of the "Wallops 2000" strategic plan, initiated in 1997,
which provides a vision for Wallops to ensure its stability and
vitality in the future. The majority of NASA civil service
engineers and technicians working on the sounding rocket program
will transition to advanced research and development projects
including Space Shuttle small payloads, the ultra-long duration
balloon program, and the University-class Explorer satellite
program, as well as management of the new contract. Wallops will
continue to manage the sounding rocket program for the Office of
Space Science, NASA Headquarters, Washington, DC.
- end -
Hа сегодня все, пока!
=SANA=
Дата: 02 декабря 1998 (1998-12-02)
От: Alexander Bondugin
Тема: Leap Second Scheduled for New Year's Eve (Forwarded)
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National Institute of Standards and Technology
Gaithersburg, Maryland
Media Contact:
Collier Smith (Boulder), (303) 497-3198
December 1998
Leap Second Scheduled for New Year's Eve
On December 31, 1998, a leap second will be inserted into the world's
Coordinated Universal Time scale, known as UTC, to keep it synchronized with
the rotation of the Earth. The leap second will be added to the last minute
before 7 p.m. EST, 6 p.m. CST, 5 p.m. MST and 4 p.m. PST, making that minute
61 seconds long. This adjustment will be made to precise clocks all over the
world that keep UTC time or local time based on UTC. In the U.S., UTC is kept
by the National Institute of Standards and Technology and the U.S. Naval
Observatory.
See http://www.boulder.nist.gov/timefreq/faq/faq.htm for more information.
You can call (303) 499-7111 to hear NIST's correct time announcement.
The Second Sprung
By David Lovering
In UTC at midnight
On December Thirty-One,
You'll find you get an extra
Second full of fun.
If you're not in Greenwich England
When the moment comes about,
You'll need to make adjustments
To the interval in doubt
At seven in the evening
(For those on EST),
Or six p.m. in Central,
Or five for MST.
Or four p.m. Pacific
Or wherever you may be,
Please thank your friendly NISTite
In Time and Frequency!
For our globe is spinning slower
(As we all are, I'm afraid),
While the Earth Rotation Service
Notes the seconds it's delayed.
Since we cannot speed the planet
We must compensate the clock,
And leap an extra second
To match our slowing rock.
(David Lovering, an electronics engineer in NIST's Information Technology
Laboratory, has a penchant for poetry.)
Andrew Yee
ayee@nova.astro.utoronto.ca
Hа сегодня все, пока!
=SANA=
Дата: 02 декабря 1998 (1998-12-02)
От: Alexander Bondugin
Тема: Case Western Reserve University's Nassau telescope goes online in Dece
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Case Western Reserve University
Cleveland, Ohio
For more information, contact:
Susan Griffith, 216-368-1004 or sbg4@po.cwru.edu.
12-1-98
CWRU's Nassau telescope goes online in December for public use
The whole world will soon have the stars and galaxies at its finger tips.
The 0.9-meter telescope at Case Western Reserve University's Nassau
Astronomical Station will go online by December 15 as the country's first
Earth-bound robotic telescope accessible to the public. Amateur and
professional astronomers alike can access the telescope by filing a viewing
request through http://astrwww.cwru.edu/nassau/nassau.html.
The first online astronomers will help CWRU debug and refine the telescope
operations, says Earle Luck, professor and chair of CWRU's Department of
Astronomy.
The robotic telescope will provide two ways of viewing images. The primary
viewing mode will be deeper images taken with main observing instrumentation
of the telescope. The other is a quick look through finder telescope. These
quick images will be posted in real time to allow a browser to see where the
telescope is pointed by the main observation request.
"You can put the telescope wherever you want in the observable sky as far as
the software and hardware are concerned," he adds. The requests can range
for viewing time from a fraction of a second to five minutes and can be a
request for a simple image to images using colored filters in red, green,
or blue.
Users also will need to provide the position of the object to be observed.
This information is available through online astronomy catalogues, also
linked to the site. As the site develops, Luck plans to add more
user-friendly information to make it easier for all to access the telescope.
Luck conceived the idea of robotizing the telescope. The reflector telescope
at the Nassau Station is one of three telescopes operated by CWRU's
Department of Astronomy. The Nassau Station is situated on one of the
highest hills in Ohio's Geauga County, approximately 30 miles east of
Cleveland.
The robotic telescope is composed of the telescope and its associated
instrumentation (camera and finder-guider), weather station, weather camera,
and power controls for the dome. Each has its own software, which feeds
information into a master control program. A computer-based scheduler in the
Department of Astronomy will coordinate the requests and return the
completed images and information to the telescope users.
By mid-1999, a robotic spectrograph will also go online for those interested
in information such as the chemical compositions of stars, how fast a star
or galaxy is moving, and the temperature of the viewed object.
Linked to the telescope is a camera trained on Polaris (the North Star), in
the direction of Lake Erie. The lake affects much of Northeast Ohio's
weather conditions. If the Polaris monitor generates an all-clear signal for
30 minutes straight, the master controller will instruct the dome to open.
Weather will be monitored every two minutes, with the dome closing in event
of high humidity, rain, snow, extreme cold, or winds of 40 mph, any of which
may damage the telescope's mirrors.
Because the station is located in a snow belt, Luck said the tricky part of
installing weather equipment was to detect snow. He solved the problem by
installing the snow detectors used to trigger the electric elements to melt
snow from driveways.
Once the telescope has gathered the requested information, it will send a
message to the telescope user that the observation is completed, with a link
to a Web-accessible file of the images. A monitoring camera with a larger
field of view is planned, which will look in the director of the requested
image. Images from this camera will be posted in real time to the Nassau
Station Web site.
The robotic telescope project received the support from the Martha Holden
Jennings Foundation in Cleveland, the Case Alumni Association, the Offices
of the CWRU President and Provost, and several private donors.
The telescope will become a teaching tool within the next year for area
teachers as part of the Hands-On Universe science program to enable middle
and high school students to learn math and physics through astronomy. The
Hands-On Universe program from the Lawrence Berkeley National Laboratory is
among a number of CWRU-community collaborations in the College of Arts and
Sciences' Center for Science and Math Education, seeking to boost interests
in these areas through discovery-based learning.
Andrew Yee
ayee@nova.astro.utoronto.ca
Hа сегодня все, пока!
=SANA=
Дата: 02 декабря 1998 (1998-12-02)
От: Alexander Bondugin
Тема: Space Shuttle Launches Super Satellite (Forwarded)
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Air Force Research Laboratory Public Affairs
CONTACT: John Brownlee
PHONE: (505) 853-3515
VS RELEASE NO. 98-41 November 25, 1998
Space Shuttle Launches Super Satellite
KIRTLAND AIR FORCE BASE, N.M. -- The Space Shuttle Endeavour will launch the
latest in Air Force Research Laboratory (AFRL) satellite experiments on
Thursday (Dec. 3) on a one-year mission to demonstrate how well five new
space technologies will work in space.
Dubbed MightySat I, this research vehicle is expected to help revolutionize
subsystem components and how they will operate in the future. It is the first
in a coming series of highly sophisticated Air Force demonstration platforms
scientists and engineers will use to quickly integrate diverse, cutting-
edge space technologies developed in the laboratory -- and expedite their
transition into actual satellites built for the warfighter.
According to 1st Lt. Barbara Braun of AFRL's Space Vehicles Directorate, the
135-pound MightySat I is a low-cost satellite about the size of a tabletop
television that will evaluate five payloads. "It is the first satellite to
be built and tested here at Kirtland AFB," she said.
"One of our experiments involves the first composite satellite bus, or
chassis, to be launched from the shuttle," Braun explained. "It makes up
most of the MightySat I satellite itself. Extremely strong, it weighs a mere
17 pounds compared to the 32-pound aluminum counterpart typically used. And
less weight means lower launch costs -- always an important consideration in
our business that spends tens of thousands of dollars for every pound put
into orbit."
"MightySat I is also testing advanced dual-junction solar cells that provide
18-21 percent more power than today's state-of-the-art materials and designs.
Other on-board experiments include smaller, more-radiation-tolerant electronic
components; microparticle impact detectors; and a "shape-memory-actuated
release device" that will help engineers prepare for the coming generation
of 'kinder, gentler' payload release mechanisms that will impart much less
physical shock to sensitive payloads than current explosive charges do," she
added.
MightySat I orbital progress will be tracked here at the Air Force Space and
Missile Systems Center's Test and Evaluation Directorate.
"We are responsible for the on-orbit care and feeding of the Air Force family
of research satellites, and MightySat I is our most recent addition," said
Space Operations Engineer 1st Lt. Valerie Malley.
"Using computer software, we 'fly' the satellite from our ground control
station here and one in Virginia run by the Orbital Sciences Corporation,"
explained Malley, who is part of a joint Air Force and civilian contractor
team charting the satellite's progress.
Malley and her peers will monitor MightySat I's health as it circles the
earth and record the status of its five experiments. Her team will receive
telemetry, capture moment-by-moment data, and inform AFRL scientists
responsible for the on-board experiments how well subsystems are performing.
"During the first two weeks of the mission, known as the 'launch and early
orbit' phase, we are primarily concerned with ensuring MightySat is spinning
properly in the right orbit at the right attitude," Malley said. "Although
the satellite has no thrusters, it does have three-axis magnetometers and
torque coils that determine the attitude of the satellite and how it spins.
We want it to tumble, end over end, rather than revolve around its axis. Once
we do that, we will begin switching on MightySat's experiments. We also will
keep in close contact with AFRL's people running the experiments. It should
be an interesting mission for us!"
PHOTO CAPTION: [http://www.vs.afrl.af.mil/news/98-41.html]
Air Force Research Laboratory technicians prepare MightySat I for pre-launch
tests.
Andrew Yee
ayee@nova.astro.utoronto.ca
Hа сегодня все, пока!
=SANA=
Дата: 02 декабря 1998 (1998-12-02)
От: Alexander Bondugin
Тема: A VLT Snapshot of Jupiter/[VLT] ISAAC observes Jupiter Occultation (Fo
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ESO Education and Public Relations Dept.
Text with all links is available on the ESO Website at URL:
http://www.eso.org/outreach/press-rel/pr-1998/phot-49-98.html
ESO Press Photo 49/98
For immediate release: 26 November 1998
A VLT Snapshot of Jupiter
The "UT1 First Light" observations in May 1998 were done with the VLT Test
Camera (TC) mounted at the Cassegrain focus of the first 8.2-m VLT Unit
Telescope. The TC was taken off the telescope in early September 1998 to
allow mounting of the FORS1 instrument at this focus. In the second half of
October, the TC was installed at Nasmyth Focus A of VLT UT1. Various test
exposures were then made for optical alignment which also served to gain
valuable experience in handling of the telescope in Nasmyth mode. This work
led up to the installation of the ISAAC instrument at the Nasmyth Focus B in
mid-November.
ESO PR Photo 49/98
PR Photo 49/98 is a reproduction of an image of giant planet Jupiter
obtained through a narrow optical filter with the VLT Test Camera at UT1
Nasmyth Focus A on October 31, 1998, at 02:06:01.0 UT in the morning. It
looks somewhat different from most other published images because of the
special passband. In terms of visible detail, it is probably one of the
best Jupiter images ever obtained with a ground-based astronomical
telescope. Just before the observation, Jupiter's large inner moon Io had
begun to pass in front of Jupiter's disk (bright spot at the lower left).
The bands in the atmosphere are well visible, also in this narrow-band
image and the "Great Red Spot" is at the right edge in the main southern
band. At this time, Jupiter was 636 million km from the Earth and the
angular diameter was about 45 arcsec.
Technical Information: The image was obtained during a period of good
seeing (0.4 arcsec). In view of the brightness of this planet (magnitude
-2.7) and the enormous light-gathering capacity of the VLT UT1, the exposure
had to be done through a narrow interference filter (H-alpha -- centered at
6562 Angstrom and FWHM 50 Angstrom) and it lasted only 0.1 second. The disc
of the planet is much darker at the edge than close to the centre which
makes an image such as this hard to display. To avoid this problem, an
unsharp-mask was applied and to enhance the contrast and sharpness of the
surface detail the image was further processed using the Lucy-Richardson
method. A bright circle to the right and some fainter ones in the same area
are artifacts. North is up and East is left.
This is the caption to ESO PR Photo 49/98. It may be reproduced, if credit
is given to the European Southern Observatory.
More information about the VLT project is available at:
URL: http://www.eso.org/outreach/info-events/ut1fl/
Copyright ESO Education & Public Relations Department
Karl-Schwarzschild-Strasse 2, D-85748 Garching, Germany
*****
ESO Education and Public Relations Dept.
Text with all links is available on the ESO Website at URL:
http://www.eso.org/outreach/press-rel/pr-1998/vid-07-98.html
ESO PR Video Clips 07a-b/98
For immediate release: 1 December 1998
ISAAC observes Jupiter Occultation
"Fly" with the VLT over the Moon's surface
A few days after the "First Light" of the VLT Infrared Spectrometer And
Array Camera (ISAAC) at the first 8.2-m VLT Unit Telescope (UT1), cf. ESO PR
19/98, the ESO Team of astronomers and engineers at Paranal have succeeded
in observing a lunar occultation of Jupiter with the new instrument. During
this event, that took place on 28 November 1998, the dark rim of the Moon's
disk moved in front of the planet, covering it from view. Somewhat later,
Jupiter reappeared behind the opposite, illuminated rim.
The ISAAC Team made use of this occasion to perform further test
observations with ISAAC and the 8.2-m VLT UT1. For this, short exposures
were made at the ISAAC Long Wavelength arm through a narrow band (1.5%)
filter centred at wavelength 3.2 microns. They lasted 4 sec during the early
phase of the occultation and decreased to 0.8 sec, then 0.4 and finally 0.08
sec, as progressively brighter areas of the illuminated part of the Moon's
surface moved into the field-of-view.
The infrared frames are presented here as two video clips.
ESO PR Video Clip 07a/98
Occultation of Jupiter on November 28, 1998:
The Moon moves in front of Jupiter's disk
[MPEG/Video; 26 frames - 184k]
The first, short sequence shows the first phase of the occultation
(ingress) during which the dark Moon rim (upper left) covers Jupiter's
disk. The bands in the planet atmosphere are well visible, and the polar
areas are bright at this infrared wavelength. In this and the following
video, the Moon moves from left to right, corresponding to West-to-East in
the sky.
ESO PR Video Clip 07b/98
Occultation of Jupiter on November 28, 1998:
"Flying" above the Moon's surface
[MPEG/Video; 266 frames - 1.1 Mb]
The second sequence consists of frames taken between 00:47:38 and 02:01:09
hrs Universal Time (UT) -- it also includes the ingress sequence shown in
Video Clip 07a/98. During this period, the telescope followed the motion
of Jupiter, while the Moon moved in front of the planet.
The visual effect is that of a "flight" over the Moon's surface. The
sequence begins at the dark side and soon moves over the terminator that
separates "day" and "night" on the Moon. Here the shadows are long and the
lunar surface relief is particularly well visible. Various craters pass by
as the surface brightness continues to increase. At the end, Jupiter
re-emerges (the egress phase) behind the bright Moon rim. Due to the
sudden change of illumination, exposure time problems were encountered at
this moment.
More about Occultations
Astronomers talk about an occultation when one celestial body moves in front
of ("hides") another, as seen by an observer at a particular site. In this
sense, total Solar and Lunar eclipses are also occultations, although this
term is not used for such events. When the Moon moves in front of a star of
a planet, one speaks about a lunar occultation; when a planet (e.g. Jupiter
or an asteroid) moves in front of a star, it is called a planetary
occultation.
Quite a few websites are available with information about occultations.
Note, in particular, that of the International Occultation Timing
Association (IOTA) and the dedicated Sky & Telescope Occultation Page.
This is the caption to ESO PR Video Clips 07a-b/98. They may be reproduced,
if credit is given to the European Southern Observatory.
More information about the VLT project is available at URL:
http://www.eso.org/outreach/info-events/ut1fl/
Additional information about ESO videos, including various News Reels, will
be found at URL: http://www.eso.org/outreach/epr/videos/.
Copyright ESO Education & Public Relations Department
Karl-Schwarzschild-Strasse 2, D-85748 Garching, Germany
Andrew Yee
ayee@nova.astro.utoronto.ca
Hа сегодня все, пока!
=SANA=
Дата: 02 декабря 1998 (1998-12-02)
От: Alexander Bondugin
Тема: Prospecting for Helium-3 on the Moon (Forwarded)
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American Geophysical Union
Public Information Office
2000 Florida Avenue, N.W.
Washington, D.C. 20009
Tel (202) 462-6900 / FAX 202-328-0566
December 1, 1998 Contact: Harvey Leifert
AGU RELEASE NO. 98-41 (202) 939-3212
For Immediate Release hleifert@kosmos.agu.org
Prospecting for Helium-3 on the Moon
WASHINGTON, D.C. -- Future prospectors on the Moon may be assisted by
resource maps developed from research by scientists in Arizona and Hawaii.
The resources they will be seeking are not gold or diamonds, but helium-3
[3He], an isotope that is rare on Earth, but more common on the Moon.
Helium-3 is expected to be the cleanest fuel of choice for potential 21st
century fusion reactors, because its reaction is efficient and produces low
residual radioactivity.
Drs. Jeffrey R. Johnson of the U.S. Geological Survey in Flagstaff,
Arizona; Timothy S. Swindle of the University of Arizona's Lunar and
Planetary Laboratory in Tucson; and Paul G. Lucey of the University of
Hawaii's Institute of Geophysics and Planetology in Honolulu have developed
a helium-3 map of the Moon based on a combination of factors they have
analyzed. Their research will be published in a forthcoming issue of
Geophysical Research Letters, a publication of the American Geophysical
Union, as "Estimated Solar Wind-Implanted Helium-3 Distribution On The
Moon."
The factors taken into account by the researchers in mapping the likely
abundance of helium-3 in a given area are the exposure age of the Moon's
surface matter, or regolith; the relative amount of charged particles,
including helium-3, arriving from the Sun (the solar wind); and the titanium
content of the lunar soil. The mineral ilmenite [FeTiO3], composed of iron,
titanium, and oxygen, retains helium much better than other major lunar
materials. The older soils should be better sources of helium-3, they
report, because they have been exposed to the solar wind longer and contain
greater amounts of fine-grained aggregates that absorb helium-3. Also, solar
wind-implanted particles are more abundant on the far side, because the
Earth shields the Moon's near side from the solar wind for a portion of each
solar orbit.
The scientists estimate that the greatest amounts of helium-3 will be found
on the far side maria, or "seas," of the Moon, due to the higher solar wind,
and in nearside areas with high concentrations of titanium dioxide [TiO2].
Their hypothesis is based on analysis of rock samples brought back by Apollo
astronauts and mineralogic maps produced by the Clementine spacecraft. They
expect to refine their maps with new elemental composition maps produced by
the Lunar Prospector spacecraft.
###
A color figure accompanies this paper. It may be accessed on the worldwide
web at: http://www.geophys.washington.edu/Space/GRL/articles/trans/ . Click
on Document . The caption is: "Simple cylindrical projections
(left side of images corresponds to 180 West longitude; 30 degree grid
shown) of (a) solar wind fluence model; (b) Clementine 750 mm mosaic; (c)
TiO2 abundance map from Lucey et. al. (1996) displayed from 0-7 weight
percent; and (d) 3He abundance map displayed from 1-10 ppb (see text for
details)."
The GRL paper upon which this release is based will be faxed to journalists
on request to Harvey Leifert (see contact information above). It has not yet
been scheduled for a specific issue of Geophysical Research Letters, but
there is no embargo.
For further information on the science in this paper, journalists may
contact Dr. Jeffrey R. Johnson at USGS Flagstaff: Phone (520) 556-7157; fax
(520) 556-7014; email: jjohnson@flagmail.wr.usgs.gov .
Andrew Yee
ayee@nova.astro.utoronto.ca
Hа сегодня все, пока!
=SANA=
Дата: 02 декабря 1998 (1998-12-02)
От: Alexander Bondugin
Тема: The Martian underground was safe place for early life (Forwarded)
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Stanford University
11/30/98
CONTACT: David Salisbury, News Service
(650) 725-1944; e-mail salisbury@stanford.edu
The Martian underground was safe place for early life
In the early years of the solar system, when giant chunks of rock and ice
pummeled the planets, the best place for life to survive -- if life existed
at all -- was in underground niches on Mars.
If Martian microbes existed, and survived the large impacts by hiding in the
Martian subsurface, they could have later traveled to Earth, via meteorites,
and seeded terrestrial life.
Those are two contentions put forth in a new paper by Norman H. Sleep,
professor of geophysics at Stanford, and Kevin Zahnle at NASA-Ames Research
Center in Mountain View. The paper, "Refugia from asteroid impacts on early
Mars and the early Earth," appeared in the Nov. 25 issue of the Journal of
Geophysical Research (Planetary Sciences Section).
"Early Mars may have been safer than the early Earth and probably was
habitable," Sleep says. That's because of the Red Planet's smaller size and
lack of large oceans. Earth's oceans, critical for supporting life under
normal conditions, may have been the planet's greatest liability in the
event of a really large impact -- a so-called "ocean-boiling impact,"
according to Sleep and Zahnle.
Between about 3.8 billion and 4.5 billion years ago, no place in the solar
system was safe from the huge arsenal of asteroids and comets left over
from the formation of the planets. Sleep and Zahnle calculate that Earth was
probably hit repeatedly by objects up to 500 kilometers across -- the distance
from Los Angeles to San Francisco. Objects that big probably missed Mars
altogether, because it was a smaller target. But if they did hit, the damage
would have been less severe, because Mars lacked large oceans to convert to
a thick, long-lasting and sterilizing steam atmosphere.
If primitive life was wiped out, possibly repeatedly, on Earth, but managed
to survive on Mars, it would not have been hard for Martian life to re-seed
Earth. Recent computer simulations have shown that, during this early period,
large amounts of material must have been exchanged between the two planets.
Some of the material blasted from Earth in meteoritic impacts would have
landed on Mars, and vice versa. Even today, a Martian meteorite hits Earth
about once every three days, Sleep says. Several billion years ago, the
impact rate was a thousand times greater. That means millions of Martian
meteorites made the trip from Mars to Earth in just a few years, a short
enough period for spores or possibly even intact microorganisms buried deep
in the meteorites to survive, he calculates.
Sleep notes that even modest-sized impacts have been known to decimate life
on Earth. The asteroid that caused the mass extinction at the end of the
Cretaceous Period was only 10 to 20 kilometers across -- small by early solar
system standards. Yet, when it hit the Yucatan peninsula 65 million years
ago, it ignited a fireball that spread out across most of North America and
launched tremendous amounts of pulverized rock almost into orbit. As that
rock dust fell back to Earth, enough heat was released to set forest fires
worldwide and to evaporate about a meter of water from the world's oceans,
Sleep says. The dinosaurs were cooked -- literally.
That is mild compared to the damage from an object hundreds of kilometers
across, like those that were hurtling through space about 4 billion years ago.
Hit the Earth with a 500-kilometer wide asteroid, and it vaporizes the rocks
at the site of impact and creates a rock-vapor atmosphere that would radiate
at temperatures of 2,000 degrees Celsius, like a star, Sleep says.
Such tremendous heat would boil off all the world's oceans and create a steam
atmosphere that would persist for about 3,000 years. That is long enough to
sterilize the Earth's outer crust down to nearly one kilometer, according to
Sleep and Zahnle. The planet is, in effect, steam-cleaned.
On Mars, an object 500 kilometers across would vaporize the rock at the site
of impact, as on Earth, but no long-lasting steam atmosphere would result, so
the thermal radiation would dissipate much more quickly. Only the upper few
hundred meters of the planet would be sterilized, compared to the upper one
kilometer on Earth, Sleep and Zahnle say.
What, if any, forms of life could have survived such devastation? Sleep and
Zahnle think the logical answer is the thermophilic -- that's Greek for heat-
loving -- organisms. Modern thermophilic organisms thrive at temperatures up
to about 100 degrees Celsius on Earth, Sleep says.
Such critters might have survived at a depth of about one kilometer
underground during the largest impacts on Earth, but the habitable zone would
have been quite narrow -- any shallower and they would have been cooked by
the energy of impact, and any deeper and they would have been cooked by
Earth's hot interior, the authors say.
By comparison, thermophilic organisms could have survived in a much broader
depth range on Mars -- from several hundred to several thousand meters below
ground, partly because of Mars' relatively cool interior, but also because of
Mars' lower gravity, which allows cracks to extend deeper into the planet's
interior and so provides living space for microbes at greater depths than on
Earth.
Sleep first began thinking about thermophilic organisms in the mid-1980s,
when colonies of these creatures were discovered in hot water vents at the
bottom of Earth's deepest oceans. Sleep imagined that such undersea vents
might provide a good refuge during asteroid impacts, because they would be
the last place to get boiled away by the intense heat of a large impact. He
reasoned that the thermophilic organisms in such niches might survive large
impacts.
Sleep thinks it is no coincidence that these creatures occupy the main trunk
on the tree of life, where the branches of more recent life are joined.
"Clearly bacteria and archaea root into thermophile organisms -- and
thermophile organisms are exactly the ones you'd expect to survive if the
ocean gets darn hot or boils," Sleep says.
The study was funded by the NASA Exobiology Program.
Andrew Yee
ayee@nova.astro.utoronto.ca
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