Tuesday, November 13, 2012
Monday, November 12, 2012
Science Alert
En busca de nuestros orÃgenes cósmicos
RADIO OBSERVATORIO ALMA
En lo alto del llano de Chajnantor, en la Cordillera de
RADIO OBSERVATORIO ALMA
En lo alto del llano de Chajnantor, en la Cordillera de
los Andes, en Chile, el Observatorio Europeo Austral (ESO), está construyendo, junto con sus socios internacionales, el Atacama Large Millimeter/submillimeter Array (ALMA), un telescopio de vanguardia para estudiar la luz de algunos de los objetos más frÃos del Universo. Esta luz tiene longitudes de onda de alrededor de un milÃmetro, entre el infrarrojo y las ondas de radio, por lo que se conoce como radiación milimétrica o submilimétrica. Se trata del mayor proyecto astronómico basado en tierra desarrollado hasta el momento.
¿Qué es la astronomÃa submilimétrica?
La luz en estas longitudes de onda proviene de grandes nubes frÃas en el espacio interestelar -a temperaturas sólo unas pocas decenas de grados por encima del cero absoluto- y de algunas de las galaxias más tempranas y distantes del Universo. Los astrónomos pueden usar dicha luz para estudiar las condiciones quÃmicas y fÃsicas que se dan en estas nubes moleculares, densas regiones de gas y polvo donde están naciendo nuevas estrellas. A menudo, estas regiones del Universo están oscurecidas y permanecen ocultas en el rango visible de la luz, pero brillan con intensidad en la parte milimétrica y submilimétrica del espectro.
La radiación milimétrica y submilimétrica abre una ventana hacia el enigmático Universo frÃo, pero el vapor de agua de la atmósfera terrestre absorbe las señales que nos llegan desde el espacio. Por ello, los telescopios de este tipo deben construirse en lugares altos y secos, de ahà que se escogiera la llanura de Chajnantor, a 5.000 metros de altitud, lo que lo convierte en uno de los observatorios astronómicos más altos de la Tierra.
¿Por qué construir ALMA en la zona alta de los Andes?
Aquà es donde ESO, junto a sus socios internacionales, está construyendo el ALMA, el mayor proyecto astronómico existente. El emplazamiento de ALMA, a unos 50 km al este de San Pedro de Atacama, en el norte de Chile, es uno de los lugares más secos de la Tierra. Allà imperan unas condiciones inmejorables para la observación, pero operar un observatorio de primera lÃnea en condiciones muy duras (altura y sequedad) supone todo un reto, ya que Chajnantor supera en unos 750 metros de altura al observatorio de Mauna Kea y en unos 2.400 metros al de Cerro Paranal, donde se ubica el Very Large Telescope (VLT).
ALMA será un telescopio único con un diseño revolucionario, compuesto inicialmente por 66 antenas de alta precisión, que operará a longitudes de onda de 0,3 a 9,6 mm. Su conjunto principal tendrá cincuenta antenas de 12 metros de diámetro cada una, que actuarán conjuntamente como un solo telescopio: un interferómetro. Esto se complementará con un compacto conjunto adicional de cuatro antenas de 12 m de diámetro y doce antenas de 7 m de diámetro. Las antenas ALMA pueden configurarse de distintas maneras, y las distancias máximas entre antenas pueden oscilar entre los 150 metros y los 16 kilómetros, lo que proporcionará a ALMA un potente "zoom" variable. Podrá sondear el universo a longitudes de onda milimétricas y submilimétricas con una sensibilidad y resolución sin precedentes, con una visión hasta diez veces más nÃtida que la del Telescopio Espacial Hubble, lo que permitirá complementar las imágenes obtenidas por el VLT.
ALMA es el telescopio más poderoso para observar el Universo frÃo, desde el gas molecular y el polvo, hasta los vestigios de la radiación del Big Bang. Estudiará los componentes básicos de las estrellas, los sistemas planetarios, las galaxias y la vida misma. Proporcionará a los cientÃficos imágenes detalladas de estrellas y planetas naciendo en nubes de gas cerca de nuestro Sistema Solar y detectará galaxias distantes en formación en los lÃmites del Universo observable, que vemos tal y como eran hace unos diez mil millones de años. De esta forma, ALMA permitirá a los astrónomos trabajar en torno a algunas de las profundas interrogantes sobre nuestros orÃgenes cósmicos.
Está previsto que la construcción de ALMA finalice alrededor del año 2013, pero las primeras observaciones cientÃficas, con parte del conjunto de telescopios, serán posibles en el 2011.
El proyecto ALMA es una colaboración entre Europa, América del Norte y Asia Oriental en cooperación con la República de Chile. ALMA está financiado en Europa por ESO, en América del Norte por la fundación Nacional de Ciencia de los Estados Unidos (NSF) en cooperación con Consejo Nacional de Investigación de Canadá (NRC) en Japón por los Institutos Nacionales de Ciencias Naturales en cooperación con la Academia Sinica (AS) en Taiwán y el consejo Nacional de Ciencias (NSC) de Taiwán. La construcción y operación de ALMA están dirigidas por ESO en representación de Europa, por el Observatorio Nacional de RadioastronomÃa (NRAO) -gestionado por Associated Universities, Inc. (AUI)- en representación de América del Norte; y por el Observatorio Astronómico Nacional de Japón (NAOJ) en representación de Asia Oriental.
Fuente. ESO
¿Qué es la astronomÃa submilimétrica?
La luz en estas longitudes de onda proviene de grandes nubes frÃas en el espacio interestelar -a temperaturas sólo unas pocas decenas de grados por encima del cero absoluto- y de algunas de las galaxias más tempranas y distantes del Universo. Los astrónomos pueden usar dicha luz para estudiar las condiciones quÃmicas y fÃsicas que se dan en estas nubes moleculares, densas regiones de gas y polvo donde están naciendo nuevas estrellas. A menudo, estas regiones del Universo están oscurecidas y permanecen ocultas en el rango visible de la luz, pero brillan con intensidad en la parte milimétrica y submilimétrica del espectro.
La radiación milimétrica y submilimétrica abre una ventana hacia el enigmático Universo frÃo, pero el vapor de agua de la atmósfera terrestre absorbe las señales que nos llegan desde el espacio. Por ello, los telescopios de este tipo deben construirse en lugares altos y secos, de ahà que se escogiera la llanura de Chajnantor, a 5.000 metros de altitud, lo que lo convierte en uno de los observatorios astronómicos más altos de la Tierra.
¿Por qué construir ALMA en la zona alta de los Andes?
Aquà es donde ESO, junto a sus socios internacionales, está construyendo el ALMA, el mayor proyecto astronómico existente. El emplazamiento de ALMA, a unos 50 km al este de San Pedro de Atacama, en el norte de Chile, es uno de los lugares más secos de la Tierra. Allà imperan unas condiciones inmejorables para la observación, pero operar un observatorio de primera lÃnea en condiciones muy duras (altura y sequedad) supone todo un reto, ya que Chajnantor supera en unos 750 metros de altura al observatorio de Mauna Kea y en unos 2.400 metros al de Cerro Paranal, donde se ubica el Very Large Telescope (VLT).
ALMA será un telescopio único con un diseño revolucionario, compuesto inicialmente por 66 antenas de alta precisión, que operará a longitudes de onda de 0,3 a 9,6 mm. Su conjunto principal tendrá cincuenta antenas de 12 metros de diámetro cada una, que actuarán conjuntamente como un solo telescopio: un interferómetro. Esto se complementará con un compacto conjunto adicional de cuatro antenas de 12 m de diámetro y doce antenas de 7 m de diámetro. Las antenas ALMA pueden configurarse de distintas maneras, y las distancias máximas entre antenas pueden oscilar entre los 150 metros y los 16 kilómetros, lo que proporcionará a ALMA un potente "zoom" variable. Podrá sondear el universo a longitudes de onda milimétricas y submilimétricas con una sensibilidad y resolución sin precedentes, con una visión hasta diez veces más nÃtida que la del Telescopio Espacial Hubble, lo que permitirá complementar las imágenes obtenidas por el VLT.
ALMA es el telescopio más poderoso para observar el Universo frÃo, desde el gas molecular y el polvo, hasta los vestigios de la radiación del Big Bang. Estudiará los componentes básicos de las estrellas, los sistemas planetarios, las galaxias y la vida misma. Proporcionará a los cientÃficos imágenes detalladas de estrellas y planetas naciendo en nubes de gas cerca de nuestro Sistema Solar y detectará galaxias distantes en formación en los lÃmites del Universo observable, que vemos tal y como eran hace unos diez mil millones de años. De esta forma, ALMA permitirá a los astrónomos trabajar en torno a algunas de las profundas interrogantes sobre nuestros orÃgenes cósmicos.
Está previsto que la construcción de ALMA finalice alrededor del año 2013, pero las primeras observaciones cientÃficas, con parte del conjunto de telescopios, serán posibles en el 2011.
El proyecto ALMA es una colaboración entre Europa, América del Norte y Asia Oriental en cooperación con la República de Chile. ALMA está financiado en Europa por ESO, en América del Norte por la fundación Nacional de Ciencia de los Estados Unidos (NSF) en cooperación con Consejo Nacional de Investigación de Canadá (NRC) en Japón por los Institutos Nacionales de Ciencias Naturales en cooperación con la Academia Sinica (AS) en Taiwán y el consejo Nacional de Ciencias (NSC) de Taiwán. La construcción y operación de ALMA están dirigidas por ESO en representación de Europa, por el Observatorio Nacional de RadioastronomÃa (NRAO) -gestionado por Associated Universities, Inc. (AUI)- en representación de América del Norte; y por el Observatorio Astronómico Nacional de Japón (NAOJ) en representación de Asia Oriental.
Fuente. ESO
New Think From NASA...
The Eagle Nebula (M16): Peering Into the Pillars Of Creation
A new look at the famous "Pillars of Creation" with NASA's Chandra X-ray Observatory has allowed astronomers to peer inside the dark columns of gas and dust. This penetrating view of the central region of the Eagle Nebula reveals how much star formation is happening inside these iconic structures.
The Chandra data shows bright X-ray so
A new look at the famous "Pillars of Creation" with NASA's Chandra X-ray Observatory has allowed astronomers to peer inside the dark columns of gas and dust. This penetrating view of the central region of the Eagle Nebula reveals how much star formation is happening inside these iconic structures.
The Chandra data shows bright X-ray so
urces in this field, most of which are young stars. In this image, red, green, and blue represent low, medium, and high energy X-rays. The Chandra data have been overlaid on the Hubble Space Telescope image to show the context of these X-ray data.
Very few X-ray sources are found in the pillars themselves. This suggests that the Eagle Nebula may be past its star-forming prime, since young stars are usually bright X-ray sources. However, there are two X-ray objects found near the tips of the pillars. One is a young star about 4 or 5 times as massive as the Sun, visible as the blue source near the tip of the pillar on the left. The other is a lower mass star near the top of the other pillar that is so faint it is not visible in the composite image.
The Chandra observations did not detect X-rays from any of the so-called evaporating gaseous globules, or EGGs. The EGGs are dense, compact pockets of interstellar gas where stars are believed to be forming. The lack of X-rays from these objects may mean that most of the EGGs do not contain enshrouded stars. However, infrared observations have shown that 11 of the 73 EGGs contain infant stellar objects and 4 of these are massive enough to form a star. The stars embedded in these 4 EGGs might be so young that they have not generated X-rays yet and one of them (E42) - estimated to have about the mass of the Sun - could represent one of the earliest stages of evolution of our nearest star. The Sun was likely born in a region like the Pillars of Creation.
The pillars and the few stars forming inside them are the last vestiges of star formation in the Eagle Nebula, also known as M16, which peaked several million years earlier. This contrasts strongly with the active star forming regions in other clusters such as NGC 2024, where Chandra sees a dense cluster of embedded young stars.
The results were published in the January 1st issue of The Astrophysical Journal and the research team, led by Jeffrey Linsky of the University of Colorado, includes Marc Gagne and Anna Mytyk (West Chester University), Mark McCaughrean (University of Exeter) and Morten Andersen (University of Arizona).
Fast Facts for The Eagle Nebula (M16):
Credit X-ray: NASA/CXC/U.Colorado/
Scale: Image is 2.5 arcmin across
Category Normal Stars & Star Clusters
Coordinates (J2000) RA 18h 18m 51.79s | Dec -13º 49' 54.93"
Constellation Serpens
Observation Date 30 Jul 01
Observation Time 22 hours
Obs. ID 978
Color Code X-ray: Red(0.5-1.5 keV); Green(1.5-2.5 keV); Blue(2.5-7.0 keV)
Instrument ACIS
References Linsky et al. (2007), ApJ, 654, 347
Distance Estimate About 7,000 light years
Release Date February 15, 2007
Very few X-ray sources are found in the pillars themselves. This suggests that the Eagle Nebula may be past its star-forming prime, since young stars are usually bright X-ray sources. However, there are two X-ray objects found near the tips of the pillars. One is a young star about 4 or 5 times as massive as the Sun, visible as the blue source near the tip of the pillar on the left. The other is a lower mass star near the top of the other pillar that is so faint it is not visible in the composite image.
The Chandra observations did not detect X-rays from any of the so-called evaporating gaseous globules, or EGGs. The EGGs are dense, compact pockets of interstellar gas where stars are believed to be forming. The lack of X-rays from these objects may mean that most of the EGGs do not contain enshrouded stars. However, infrared observations have shown that 11 of the 73 EGGs contain infant stellar objects and 4 of these are massive enough to form a star. The stars embedded in these 4 EGGs might be so young that they have not generated X-rays yet and one of them (E42) - estimated to have about the mass of the Sun - could represent one of the earliest stages of evolution of our nearest star. The Sun was likely born in a region like the Pillars of Creation.
The pillars and the few stars forming inside them are the last vestiges of star formation in the Eagle Nebula, also known as M16, which peaked several million years earlier. This contrasts strongly with the active star forming regions in other clusters such as NGC 2024, where Chandra sees a dense cluster of embedded young stars.
The results were published in the January 1st issue of The Astrophysical Journal and the research team, led by Jeffrey Linsky of the University of Colorado, includes Marc Gagne and Anna Mytyk (West Chester University), Mark McCaughrean (University of Exeter) and Morten Andersen (University of Arizona).
Fast Facts for The Eagle Nebula (M16):
Credit X-ray: NASA/CXC/U.Colorado/
Scale: Image is 2.5 arcmin across
Category Normal Stars & Star Clusters
Coordinates (J2000) RA 18h 18m 51.79s | Dec -13º 49' 54.93"
Constellation Serpens
Observation Date 30 Jul 01
Observation Time 22 hours
Obs. ID 978
Color Code X-ray: Red(0.5-1.5 keV); Green(1.5-2.5 keV); Blue(2.5-7.0 keV)
Instrument ACIS
References Linsky et al. (2007), ApJ, 654, 347
Distance Estimate About 7,000 light years
Release Date February 15, 2007
Cygnus OB2: Probing a Nearby Stellar Cradle
Cygnus OB2 is a star cluster in the Milky Way that contains many hot, massive young stars.
This composite image of Cygnus OB2 contains X-rays from Chandra (blue), infrared data from Spitzer (red), and optical data from the Isaac Newton Telescope (orange).
Astronomers would like to better understand how this and other star factories like it form and evolve.
A deep Chandra observation of Cygnus OB2 has found almost 1,500 stars emitting X-rays.
The Milky Way and other galaxies in the universe harbor many young star clusters and associations that each contain hundreds to thousands of hot, massive, young stars known as O and B stars. The star cluster Cygnus OB2 contains more than 60 O-type stars and about a thousand B-type stars. At a relatively nearby distance to Earth of about 5,000 light years, Cygnus OB2 is the closest massive cluster. Deep observations with NASA's Chandra X-ray Observatory of Cygnus OB2 have been used to detect the X-ray emission from the hot outer atmospheres, or coronas, of young stars in the cluster and to probe how these great star factories form and evolve. About 1,700 X-ray sources were detected, including about 1,450 thought to be stars in the cluster. In this image, X-rays from Chandra (blue) have been combined with infrared data from NASA's Spitzer Space Telescope (red) and optical data from the Isaac Newton Telescope (orange).
Young stars ranging in age from one million to seven million years were detected. The infrared data indicates that a very low fraction of the stars have circumstellar disks of dust and gas. Even fewer disks were found close to the massive OB stars, betraying the corrosive power of their intense radiation that leads to early destruction of their disks. Evidence is also seen that the older population of stars has lost its most massive members because of supernova explosions. Finally, a total mass of about 30,000 times the mass of the sun is derived for Cygnus OB2, similar to that of the most massive star forming regions in our Galaxy.
Fast Facts for Cygnus OB2:
Credit X-ray: NASA/CXC/SAO/J.Drake et al, Optical: Univ. of Hertfordshire/INT/IPHAS, Infrared: NASA/JPL-Caltech
Release Date : November 7, 2012
Scale Image is 11.8 arcmin across (16 light years)
Category: Normal Stars & Star Clusters
Coordinates (J2000) RA 20h 37m 11.00s | Dec +38° 41' 52.00"
Constellation: Cygnus
Observation Date: 39 pointings between January 2004 and March 2010
Observation Tim : 341 hours 40 min (14 days 5 hours 40 min)
Obs. ID 4501, 4511, 10939-10974, 12099
Instrument: ACIS
Color Code X-ray (Blue), Optical (Yellow), Infrared (Red)
Distance Estimate: About 4,700 light year
Cygnus OB2 is a star cluster in the Milky Way that contains many hot, massive young stars.
This composite image of Cygnus OB2 contains X-rays from Chandra (blue), infrared data from Spitzer (red), and optical data from the Isaac Newton Telescope (orange).
Astronomers would like to better understand how this and other star factories like it form and evolve.
A deep Chandra observation of Cygnus OB2 has found almost 1,500 stars emitting X-rays.
The Milky Way and other galaxies in the universe harbor many young star clusters and associations that each contain hundreds to thousands of hot, massive, young stars known as O and B stars. The star cluster Cygnus OB2 contains more than 60 O-type stars and about a thousand B-type stars. At a relatively nearby distance to Earth of about 5,000 light years, Cygnus OB2 is the closest massive cluster. Deep observations with NASA's Chandra X-ray Observatory of Cygnus OB2 have been used to detect the X-ray emission from the hot outer atmospheres, or coronas, of young stars in the cluster and to probe how these great star factories form and evolve. About 1,700 X-ray sources were detected, including about 1,450 thought to be stars in the cluster. In this image, X-rays from Chandra (blue) have been combined with infrared data from NASA's Spitzer Space Telescope (red) and optical data from the Isaac Newton Telescope (orange).
Young stars ranging in age from one million to seven million years were detected. The infrared data indicates that a very low fraction of the stars have circumstellar disks of dust and gas. Even fewer disks were found close to the massive OB stars, betraying the corrosive power of their intense radiation that leads to early destruction of their disks. Evidence is also seen that the older population of stars has lost its most massive members because of supernova explosions. Finally, a total mass of about 30,000 times the mass of the sun is derived for Cygnus OB2, similar to that of the most massive star forming regions in our Galaxy.
Fast Facts for Cygnus OB2:
Credit X-ray: NASA/CXC/SAO/J.Drake et al, Optical: Univ. of Hertfordshire/INT/IPHAS, Infrared: NASA/JPL-Caltech
Release Date : November 7, 2012
Scale Image is 11.8 arcmin across (16 light years)
Category: Normal Stars & Star Clusters
Coordinates (J2000) RA 20h 37m 11.00s | Dec +38° 41' 52.00"
Constellation: Cygnus
Observation Date: 39 pointings between January 2004 and March 2010
Observation Tim : 341 hours 40 min (14 days 5 hours 40 min)
Obs. ID 4501, 4511, 10939-10974, 12099
Instrument: ACIS
Color Code X-ray (Blue), Optical (Yellow), Infrared (Red)
Distance Estimate: About 4,700 light year
Stellar Evolution with Type 1a Supernova Remnant
This tableau illustrates the ongoing drama of stellar evolution, and how the rate of evolution and the ultimate fate of a star depends on its weight, or mass. (Illustration:
This graphic gives a summary of our best current understanding of the evolution of stars, showing their birth, middle age and eventual demise. The lowest mass stars are shown
This tableau illustrates the ongoing drama of stellar evolution, and how the rate of evolution and the ultimate fate of a star depends on its weight, or mass. (Illustration:
This graphic gives a summary of our best current understanding of the evolution of stars, showing their birth, middle age and eventual demise. The lowest mass stars are shown
at the bottom and the highest mass stars at the top. The very top line is a relatively recent addition compelled by the detection of SN 2006gy, that describes the evolution of the most massive stars in the universe. Observational evidence for the special type of explosion shown here - which is incredibly bright and obliterates the star rather than producing a black hole - was lacking until SN 2006gy was found.
Pelican Nebula Close-up
The prominent ridge of emission featured in this vivid skyscape is designated IC 5067. Part of a larger emission nebula with a distinctive shape, popularly called The Pelican Nebula, the ridge spans about 10 light-years and follows the curve of the cosmic pelican's head and neck. Fantastic, dark shapes inhabiting the view are clouds of cool gas and dust sculpted by energe
tic radiation from hot, massive stars. But stars are also forming within the dark shapes. In fact, twin jets emerging from the tip of the central, dark tendril are the telltale signs of an embedded protostar cataloged as Herbig-Haro 555. The Pelican Nebula itself, also known as IC 5070, is about 2,000 light-years away. To find it, look northeast of bright star Deneb in the high flying constellation Cygnus.
Tuesday, November 6, 2012
Science Alert
Voting from space? Astronauts aboard the International Space Station (ISS) are getting ready to cast their vote in the 2012 US Presidential Election. Mission Control at NASA's Johnson Space Center in Houston will send a digital ballot to the astronauts; they will fill it out and then send it back to Earth along the same path.
Geckos have tiny hair-like structures on their feet that work almost like Velcro, allowing them to adhere and climb vertical surfaces.
Bariatric surgery has proven to be an effective tool against obesity and obesity related diseases, but new research suggests that some types of bariatric surgery could have an impact on bone health. Scientists studied the relationship between fat, bone and nutritional restrictions and discovered that some surgery-induced changes, including rapid weight loss, may have an impact on nutrient absorption and hormone production, which affects bone strength. The researchers suggest monitoring bone health before and after the procedure.
The elusive spade-toothed beaked whale remained a mystery for marine biologists until 2010, when two specimens beached in the Bay of Plenty, New Zealand. After extensive DNA analysis, scientists confirmed that those complete specimens were the first animals of their kind ever seen, previous evidence of their existence consisted only of skull and jaw fragments [pictured]. The world’s rarest and most enigmatic whale could already be endangered.
Thursday, November 1, 2012
From NASA
Protective Paint Tested on Space Station Makes for 'Curious' Ride to Mars
This photo shows the coated fins, center, on Curiosity's Multi-Mission Radioisotope Thermoelectric Generator. The protective coating on the fins was tested as part of the MISSE-2 investigation aboard the International Space Station. (NASA)
A coating that survived long-term exposure on the International Space Station took a
This photo shows the coated fins, center, on Curiosity's Multi-Mission Radioisotope Thermoelectric Generator. The protective coating on the fins was tested as part of the MISSE-2 investigation aboard the International Space Station. (NASA)
A coating that survived long-term exposure on the International Space Station took a
n
even longer journey on the Mars Curiosity Rover and is protecting the
craft's critical power unit as it collects data on Mars. Not all space
environments are the same, but if a material can survive for a long time
in one space environment, it may prove useful for longer exploration
missions.
Curiosity's paint-like spray coating, AZ-2100-IECW, was exposed to the harsh space environment for four years as part of the Materials on International Space Station Experiment (MISSE) investigation. The coating, tested and developed by AZ Technology in Huntsville, Ala., met stringent outgassing requirements and withstood temperature extremes and thousands of hours of ultraviolet radiation from the sun, making it an ideal candidate for the cooling fins on Curiosity's power unit.
"It's exciting to be part of the Mars Science Laboratory mission and see our work on the surface of Mars," said Lynn Leeper, AZ Technology president and chief executive officer. AZ Technology has been developing spacecraft paint and coatings for more than 20 years and has been involved in a number of successful spacecraft and space materials experiments. The company provided 19 different paints, including the AZ-2100-IECW, for the MISSE-2 investigation, which flew from August 2001 to July 2005.
The MISSE materials test bed has provided data on the durability of materials that have helped spacecraft designers shorten the development time for satellite hardware components by 50%. Shorter development times result in more affordable spacecraft and ensure materials perform as expected in challenging space environments.
The EC in the coating used for Curiosity stands for electrically conductive. Static electricity can build up on a spacecraft as it is exposed to proton and electron radiation. Electrically conductive or static-dissipative coatings can help protect the electronics from getting zapped. AZ Technology's coating was applied on the Multi-Mission Radioisotope Thermoelectric Generator, or MMRTG. This power unit converts the heat from decaying plutonium-238 into electricity that the Curiosity rover needs to survive.
"Our company has coated parts for many satellites, the International Space Station, and extra-orbital missions, but typically we do not get to see pictures of our work in such an amazing setting," added Leeper. "It makes us feel much closer to the adventure."
The potential for future exploration projects to benefit from space station technology continues to expand, thanks to ongoing use of the orbiting laboratory as a technology test bed. Currently MISSE-8 operates externally aboard the space station, continuing to aid in developing advanced materials to Mars and beyon
Curiosity's paint-like spray coating, AZ-2100-IECW, was exposed to the harsh space environment for four years as part of the Materials on International Space Station Experiment (MISSE) investigation. The coating, tested and developed by AZ Technology in Huntsville, Ala., met stringent outgassing requirements and withstood temperature extremes and thousands of hours of ultraviolet radiation from the sun, making it an ideal candidate for the cooling fins on Curiosity's power unit.
"It's exciting to be part of the Mars Science Laboratory mission and see our work on the surface of Mars," said Lynn Leeper, AZ Technology president and chief executive officer. AZ Technology has been developing spacecraft paint and coatings for more than 20 years and has been involved in a number of successful spacecraft and space materials experiments. The company provided 19 different paints, including the AZ-2100-IECW, for the MISSE-2 investigation, which flew from August 2001 to July 2005.
The MISSE materials test bed has provided data on the durability of materials that have helped spacecraft designers shorten the development time for satellite hardware components by 50%. Shorter development times result in more affordable spacecraft and ensure materials perform as expected in challenging space environments.
The EC in the coating used for Curiosity stands for electrically conductive. Static electricity can build up on a spacecraft as it is exposed to proton and electron radiation. Electrically conductive or static-dissipative coatings can help protect the electronics from getting zapped. AZ Technology's coating was applied on the Multi-Mission Radioisotope Thermoelectric Generator, or MMRTG. This power unit converts the heat from decaying plutonium-238 into electricity that the Curiosity rover needs to survive.
"Our company has coated parts for many satellites, the International Space Station, and extra-orbital missions, but typically we do not get to see pictures of our work in such an amazing setting," added Leeper. "It makes us feel much closer to the adventure."
The potential for future exploration projects to benefit from space station technology continues to expand, thanks to ongoing use of the orbiting laboratory as a technology test bed. Currently MISSE-8 operates externally aboard the space station, continuing to aid in developing advanced materials to Mars and beyon
Saturday, October 27, 2012
From NASA of Space...
NGC 604 is a H II region inside the Triangulam Galaxy. It was discovered by William Harschel on 11th Sep,1784. It is one of the largest H II regions in the Local Group of galaxies estimated distance of 2.7 million light-years it's longest diameter is roughly 1500 light-years(460 parsecs) over 40 times the size of the visible portion of the Orion Nebula. It is over 6300 times mo
re luminous than the Orion Nebula and if it were at the same distance it would out shine Venus Like all emission nebulae it's gas is ionized by a cluster of Massive stars at it's center.
This clock representation shows some of the major units of geological time and definitive events of Earth history, The Hadean eon represents the time before fossil record of life on Earth, its upper boundary is now considered as 4.0Ga. Other sub-divisions reflect the evolu
tion of life. The Archean and Proterozoic are both eons, The Palaeozoic, Mesozoic and Cenozoic are eras of the Phanerozoic eon the two million years Quaternary period. The time of recognizable humans is too small to be visible at this scale.
image credit: NASA,EST,HST, Andrew Fruchter,(STScI)and the ERO team(STScI+ST-ECF)_
NGC 2392 lies more than 2870 light year away and visible in the Constellation of Gemini._
The Eskimo Nebula(NGC 2392) ,also know as the Clownface Nebula or Caldwell 39, is a bipokar double-Shell planetary nebula. In 1787,William Harschel discovered it.
The formation resembles a person's head surrounded by a Parka hood. It is surrounded by gas that composed the other layers of a Sun-like star._
The visible inner filaments are ejected by a strong wind of particles from the central star, The outer disk,contains unusual light year long orange filaments.
so that Earth does not occult the stars which are observed continuously, and so the photometer is not influenced by stray light from Earth. This orbit avoids the gravitational perturbations and Torques inhernt in an Earth orbit, allowing for a more stable viewing platfrom.
The photometer points to a field in the Northern constellations of Cygnus, Lyra and Draco(image), which is well out of the ecliptic plane. So sunlight never enters the photometer as the spacecraft orbits the Sun,Cygnus is also a good choice to observe because it'll never be obscured by asteroid belt.
other benefit is that Keplar is pointing in the direction of the Solar system's motion around the center of the galaxy. Thus the stars which are observed by Keplar are roughly the same distance from the glactic center as the solar system and also close to the galactic plane. its important if position in the Galaxy is related to habitability as suggested by the Rare Earth hypothesis____
The photometer points to a field in the Northern constellations of Cygnus, Lyra and Draco(image), which is well out of the ecliptic plane. So sunlight never enters the photometer as the spacecraft orbits the Sun,Cygnus is also a good choice to observe because it'll never be obscured by asteroid belt.
other benefit is that Keplar is pointing in the direction of the Solar system's motion around the center of the galaxy. Thus the stars which are observed by Keplar are roughly the same distance from the glactic center as the solar system and also close to the galactic plane. its important if position in the Galaxy is related to habitability as suggested by the Rare Earth hypothesis____
Exp:what does a Coment nucleus look like?
Formed from the priomordial stuff of the solar system.It's thought to resemble a very dirty iceberg.But for active comets,telescopic images only reveal the surrounding cloud of gas n dust, the comet's coma n the characteristic cometary tails.In 1986 The ESA's Giotto encountered the necleus of Halley's comet as it approached the Sun.Data from Giotto Camera was used to generate this enhanced image of the potato shaped nucleus which measured roughly 15km across,It shows surface features on the dark nucleus against the bright background of the coma as the icy material is Vaporized by the sun's heat,Every 76yrs Halley returns to the inner solar system n each time the nucleus sheds about a 6 meter deep layer of its ice n rock into space.This debris composes Halley's tails n leaves an orbiting trail responsible for the Orionids meteor shower
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