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domingo, 19 de junio de 2016

ESA : How the Sun was born .- Así nació El Sol

Hola amigos: A VUELO DE UN QUINDE EL BLOG., hemos recibido información de la Agencia Espacial Europea ESA, dándonos detalles como nació El Sol.

ESA, nos dice: "Se puede ver como una estrella, que se puede llamar una estrella, pero todavía no generar energía como una estrella normal. Esto es porque aún se está formando esta estrella.Se ofrece una visión fascinante de nuestro propio pasado debido a nuestro Sol comienza su vida como tal una estrella 'T Tauri' hace unos 4,6 millones de años.Situado a 1800 años luz de distancia en la constelación de Cygnus, V1331 Cyg fue originalmente nada más que una nube difusa de gas en el espacio. Poco a poco con el tiempo, la gravedad ha tirado juntos, pero el proceso no ha terminado todavía. V1331 aún no está completamente formado y también lo es aún mayor de lo que con el tiempo será una vez que la gravedad ha hecho su trabajo. Se está brillando debido a la energía de ser liberado como se contrae.Eventualmente, será lo suficientemente compacta que la temperatura en su centro se encender la fusión nuclear. El hidrógeno a continuación, se transforma en helio y esto dará a conocer los torrentes de energía que harán V1331 Cyg brillar durante miles de millones de años como una estrella de buena fe.Las franjas de polvo que rodean a la estrella son los restos de la nube de la cual se condensa. A menudo, este disco circum oscurece nuestra visión del objeto estelar joven, pero, por casualidad, nos ha tocado estar mirando hacia abajo en el polo de rotación de la estrella, por lo que aparece como un rayo deslumbrante 'reflector'.Este disco circunestelar es el sitio donde los planetas pueden estar formándose, y en el caso de tiempo V1331 Cyg se está acabando. Una estrella T Tauri produce un fuerte "viento" de las partículas atómicas que disipa el disco, con lo que la formación de planetas a su fin....."La imagen fue tomada por la
• / ESA telescopio espacial Hubble de la NASA
• y es una combinación de tres exposiciones tomadas en diferentes longitudes de onda. Estos casi corresponden a la vista humana: azul, verde y, en lugar de luz roja que nuestros ojos verían, Hubble utilizó en el infrarrojo cercano.• Id 361840

More information..............
http://www.esa.int/spaceinimages/Images/2016/06/Young_star_offers_a_glimpse_of_the_Sun_s_past

Young star offers a glimpse of the Sun’s past .- Estrella joven ofrece una visión del pasado del Sol

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Details

Title Young star offers a glimpse of the Sun’s past
Released 13/06/2016 12:45 pm
Copyright ESA/Hubble, NASA, K. Stapelfeldt (GSFC), B. Stecklum & A. Choudhary (Thüringer Landessternwarte Tautenburg, Germany)
Description

It may look like a star, it may be called a star, but it does not yet generate energy like a normal star. This is because this star is still being formed.

It offers a fascinating glimpse into our own past because our Sun began its life as such a ‘T Tauri’ star some 4.6 billion years ago.

Located 1800 light-years away in the constellation Cygnus, V1331 Cyg was originally nothing but a diffuse cloud of gas in space. Slowly over time, gravity has pulled it together, but the process is not yet over. V1331 is not yet fully formed and so is still larger than it will eventually be once gravity has done its job. It is shining because of the energy being released as it shrinks.

Eventually, it will be compact enough that the temperature in its centre will ignite nuclear fusion. Hydrogen will then be transformed into helium and this will release the torrents of energy that will make V1331 Cyg shine for billions of years as a bona fide star.

The swathes of dust that surround the star are the remnants of the cloud from which it condensed. Often, this circumstellar disc obscures our view of the young stellar object but, by chance, we happen be looking down on the rotational pole of the star, so it appears as a dazzling ‘searchlight’ beam.

This circumstellar disc is the site where planets may be forming, and in the case of V1331 Cyg time is running out. A T Tauri star produces a strong ‘wind’ of atomic particles that dissipates the disc, bringing planet formation to an end.

The image was taken by the
NASA/ESA Hubble Space Telescope
and is a combination of three exposures taken at different wavelengths. These almost correspond to human eyesight: blue, green and, instead of red light that our eyes would see, Hubble used near-infrared.
Id 361840

ESA
Guillermo Gonzalo Sánchez Achutegui
ayabaca@gmail.com
ayabaca@Hotmail.com
ayabaca@yahoo.com

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jueves, 25 de diciembre de 2014

NASA : Hubble Sees the Beautiful Side of Galaxy IC 335.- Telescopio Espacial Hubble ve el lado hermoso de la galaxia IC 335

Hola amigos: A VUELO DE UN QUINDE EL BLOG., la Agencia Espacial NASA, nos informa que el Telescopio Espacial Hubble, ha captado una bella imagen de la Galaxia IC 335; Esta nueva imagen del telescopio espacial Hubble de la NASA / ESA muestra la galaxia IC 335 frente a un telón de fondo de las galaxias distantes. IC 335 es parte de un grupo de galaxias que contiene otras tres galaxias, y situado en el cúmulo de Galaxias Fornax 60 millones de años-luz de distancia.

Como se observa en esta imagen, el disco de IC 335 aparece de canto desde el punto de vista de la Tierra. Esto hace que sea más difícil para los astrónomos clasifican, ya que la mayoría de las características de la morfología de una galaxia - los brazos de una espiral o el bar de enfrente del centro - son sólo visibles en su rostro. Aún así, el 45 000 años luz de largo galaxia podría ser clasificado como un tipo SO.(http://es.wikipedia.org/wiki/Galaxia)

Estas galaxias lenticulares son un estado intermedio en sistemas de clasificación morfológica de galaxias entre cierto galaxias espirales y elípticas. Tienen un disco estelar delgada y un bulto, como las galaxias espirales, pero a diferencia de las galaxias espirales típicas que han utilizado la mayor parte del medio interestelar. Sólo unas pocas estrellas nuevas se pueden crear a partir del material que queda y la tasa de formación de estrellas es muy baja. Por lo tanto, la población de estrellas en las galaxias S0 se compone principalmente de estrellas viejas, muy similar a la población de estrellas en las galaxias elípticas.(http://es.wikipedia.org/wiki/Galaxia_lenticular)

Como galaxias S0 sólo han mal definida brazos espirales que se confunden fácilmente con las galaxias elípticas si son vistos inclinado cara o de canto como IC 335 aquí. Y, en efecto, a pesar de las diferencias morfológicas entre S0 y la clase galaxias elípticas, comparten algunas características comunes, como tamaños típicos y las características espectrales.

Ambas clases también se consideran "galaxias de tipo temprano", debido a que están evolucionando de forma pasiva. Sin embargo, mientras que las galaxias elípticas pueden ser pasivamente evolución cuando los observamos, que han tenido por lo general las interacciones violentas con otras galaxias en su pasado. Por el contrario, las galaxias S0 son o bien el envejecimiento y la decoloración galaxias espirales, que nunca tuvieron ninguna interacción con otras galaxias, o que son el resultado del envejecimiento de una única fusión entre dos galaxias espirales en el pasado. La naturaleza exacta de estas galaxias es todavía un tema de debate.

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Hubble Sees the Beautiful Side of Galaxy IC 335

This new NASA/ESA Hubble Space Telescope image shows the galaxy IC 335 in front of a backdrop of distant galaxies. IC 335 is part of a galaxy group containing three other galaxies, and located in the Fornax Galaxy Cluster 60 million light-years away.

As seen in this image, the disk of IC 335 appears edge-on from the vantage point of Earth. This makes it harder for astronomers to classify it, as most of the characteristics of a galaxy’s morphology — the arms of a spiral or the bar across the center — are only visible on its face. Still, the 45 000 light-year-long galaxy could be classified as an S0 type.

These lenticular galaxies are an intermediate state in galaxy morphological classification schemes between true spiral and elliptical galaxies. They have a thin stellar disk and a bulge, like spiral galaxies, but in contrast to typical spiral galaxies they have used up most of the interstellar medium. Only a few new stars can be created out of the material that is left and the star formation rate is very low. Hence, the population of stars in S0 galaxies consists mainly of aging stars, very similar to the star population in elliptical galaxies.

As S0 galaxies have only ill-defined spiral arms they are easily mistaken for elliptical galaxies if they are seen inclined face-on or edge-on as IC 335 here. And indeed, despite the morphological differences between S0 and elliptical class galaxies, they share some common characteristics, like typical sizes and spectral features.

Both classes are also deemed "early-type" galaxies, because they are evolving passively. However, while elliptical galaxies may be passively evolving when we observe them, they have usually had violent interactions with other galaxies in their past. In contrast, S0 galaxies are either aging and fading spiral galaxies, which never had any interactions with other galaxies, or they are the aging result of a single merger between two spiral galaxies in the past. The exact nature of these galaxies is still a matter of debate.

European Space Agency
Credit: ESA/Hubble and NASA

NASA

Guillermo Gonzalo Sánchez Achutegui

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domingo, 23 de noviembre de 2014

NASA: Mixing Paints . - Mezcla de Pinturas en los Anillos de Saturno

Hola amigos: A VUELO DE UN QUINDE EL BLOG., hemos recibido un espectacular imagen de la Agencia Espacial NASA, sobre lo que ellos llaman una "Mezcla de Pinturas en Saturno".... el arte natural de un artista esta vez parece haber dejado que sus pinturas se arremolinan juntos un poco..................

"Lo que el espectador puede percibir que sea la superficie de Saturno es realmente sólo la parte superior de sus más altas capas de nubes. Todo lo que vemos es el resultado de la dinámica de fluidos. Los astrónomos estudian dinámica de las nubes de Saturno, en parte para probar y mejorar nuestra comprensión de los flujos de fluidos. Esperemos que lo que aprendemos será útil para la comprensión de nuestra propia atmósfera y la de otros cuerpos planetarios..................

"Esta vista se dirige hacia el lado iluminado de los anillos desde unos 25 grados por encima del plano de los anillos. La imagen fue tomada en luz roja con la cámara de ángulo estrecho de Nave Cassini el 23 de agosto de 2014..........................."

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Mixing Paints

Nature is an artist, and this time she seems to have let her paints swirl together a bit.

What the viewer might perceive to be Saturn's surface is really just the tops of its uppermost cloud layers. Everything we see is the result of fluid dynamics. Astronomers study Saturn's cloud dynamics in part to test and improve our understanding of fluid flows. Hopefully, what we learn will be useful for understanding our own atmosphere and that of other planetary bodies.

This view looks toward the sunlit side of the rings from about 25 degrees above the ringplane. The image was taken in red light with the Cassini spacecraft narrow-angle camera on Aug. 23, 2014.

The view was acquired at a distance of approximately 1.1 million miles (1.8 million kilometers) from Saturn and at a Sun-Saturn-spacecraft, or phase, angle of 127 degrees. Image scale is 7 miles (11 kilometers) per pixel.

The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colo.

For more information about the Cassini-Huygens mission

visit http://www.nasa.gov/cassini

and http://saturn.jpl.nasa.gov .

The Cassini imaging team homepage is at

http://ciclops.org .

Credit: NASA/JPL-Caltech/Space Science Institute

NASA
Guillermo Gonzalo Sánchez Achutegui
ayabaca@gmail.com
ayabaca@hotmail.com
ayabaca@yahoo.com

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sábado, 15 de noviembre de 2014

NASA : Welcome to a Comet, from Lander on Surface.- Bienvenido Lander sobre el sobre el cometa.

Hola amigos : A VUELO DE UN QUINDE EL BLOG., la Agencia Espacial NASA, nos informa lo que pasó después de la gran hazaña de la Misión Rosetta al colocar la sonda: Philae sobre el cometa: Comet 67P/Churyumov-Gerasimenko, un prodigio de la tecnología espacial, fue un trabajo de la Agencia Europea del Espacio ESA.

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Welcome to a Comet, from Lander on Surface

The Philae lander of the European Space Agency's Rosetta mission is safely on the surface of Comet 67P/Churyumov-Gerasimenko, as these first two images from the lander's CIVA camera confirm. One of the lander’s three feet can be seen in the foreground. The view is a two-image mosaic taken on Nov. 12, 2014.

The lander separated from the orbiter at 09:03 UTC (1:03 a.m. PST) for touch down on comet 67P seven hours later.

Rosetta and Philae had been riding through space together for more than 10 years. Philae is the first probe to achieve soft landing on a comet, and Rosetta is the first to rendezvous with a comet and follow it around the sun. The information collected by Philae at one location on the surface will complement that collected by the Rosetta orbiter for the entire comet.

Rosetta is a European Space Agency mission with contributions from its member states and NASA. Rosetta's Philae lander is provided by a consortium led by the German Aerospace Center, Cologne; Max Planck Institute for Solar System Research, Gottingen; French National Space Agency, Paris; and the Italian Space Agency, Rome. NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology, Pasadena, manages the U.S. participation in the Rosetta mission for NASA's Science Mission Directorate in Washington. Rosetta carries three NASA instruments in its 21-instrument payload.

For more information on the U.S. instruments aboard Rosetta, visit: http://rosetta.jpl.nasa.gov . For more information about Rosetta, visit http://www.esa.int/rosetta .

NASA

Guillermo Gonzalo Sánchez Achutegui

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viernes, 14 de noviembre de 2014

NASA : Mars Spacecraft Reveal Comet Flyby Effects on Martian Atmosphere.- Las naves espaciales de Marte , revela Efectos del cometa sobrevuelo del Ambiente marciano

Hola amigos: A VUELO DE UN QUINDE EL BLOG.,la Agencia Espacial NASA, nos revela sobre los efectos que produjo sobre la atmósfera de Marte el sobrevuelo del Cometa : Comet C/2013 A1 Siding Spring, la agencia utilizó dos satélites: NASA's Mars Atmosphere and Volatile Evolution (MAVEN) misión, y NASA’s Mars Reconnaissance Orbiter (MRO), con el apoyo de la Agencia: European Space Agency (ESA) con su nave: Mars Express spacecraft.

El cometa pasó tan cerca de Marte, que NASA nos informa así: "El cometa C / 2013 A1 Siding Spring viajó desde la región más distante de nuestro sistema solar, llamada la Nube de Oort, e hizo un acercamiento cercano alrededor de 14:27 EDT dentro de aproximadamente 87.000 millas (139.500 kilometros) del planeta rojo. Esto es menos de la mitad de la distancia entre la Tierra y la Luna, y menos de una décima parte de la distancia de cualquier sobrevuelo del cometa conocido de la Tierra...

Artist’s concept of Comet Siding Spring approaching Mars, shown with NASA’s orbiters preparing to make science observations of this unique encounter.

Image Credit:

NASA/JPL

Youtube Override:

This movie begins with an animation (artist's rendering) of NASA's Mars Reconnaissance Orbiter spacecraft above Mars. The scene zooms into an "X-ray" view of the spacecraft, revealing the High Resolution Imaging Science Experiment (HiRISE) camera.

Five images of comet Siding Spring taken within a 35-minute period as it passed near Mars on Oct. 19, 2014, provide information about the size of the comet's nucleus. The images were acquired by the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter.

Image Credit:

NASA/JPL-Caltech/University of Arizona

Feature Link:

Full image and caption

These spectrograms from the MARSIS instrument on the European Space Agency's Mars Express orbiter show the intensity of radar echo in Mars' far-northern ionosphere at three times on Oct. 19 and 20, 2014. The middle plot reveals effects attributed to dust from a comet that passed near Mars that day.

Image Credit:

ASI/NASA/ESA/JPL/Univ. of Rome/Univ. of Iowa

Feature Link:

Full image and caption

Two NASA and one European spacecraft that obtained the first up-close observations of a comet flyby of Mars on Oct. 19, have gathered new information about the basic properties of the comet’s nucleus and directly detected the effects on the Martian atmosphere.

Data from observations carried out by NASA's Mars Atmosphere and Volatile Evolution (MAVEN) mission, NASA’s Mars Reconnaissance Orbiter (MRO), and a radar instrument on the European Space Agency's (ESA’s) Mars Express spacecraft have revealed that debris from the comet added a temporary and very strong layer of ions to the ionosphere, the electrically charged layer high above Mars. In these observations, scientists were able to make a direct connection from the input of debris from a specific meteor shower to the formation of this kind of transient layer in response; that is a first on any planet, including Earth.

Comet C/2013 A1 Siding Spring traveled from the most distant region of our solar system, called the Oort Cloud, and made a close approach around 2:27 p.m. EDT within about 87,000 miles (139,500 kilometers) of the Red Planet. This is less than half the distance between Earth and our moon and less than one-tenth the distance of any known comet flyby of Earth.

Dust from the comet impacted Mars and was vaporized high in the atmosphere, producing what was likely an impressive meteor shower. This debris resulted in significant temporary changes to the planet’s upper atmosphere and possible longer-term perturbations. Earth-based and a host of space telescopes also observed the unique celestial object.

“This historic event allowed us to observe the details of this fast-moving Oort Cloud comet in a way never before possible using our existing Mars missions,” said Jim Green, director of NASA’s Planetary Science Division at the agency’s Headquarters in Washington. “Observing the effects on Mars of the comet's dust slamming into the upper atmosphere makes me very happy that we decided to put our spacecraft on the other side of Mars at the peak of the dust tail passage and out of harm's way.”

The MAVEN spacecraft, recently arrived at Mars, detected the comet encounter in two ways. The remote-sensing Imaging Ultraviolet Spectrograph observed intense ultraviolet emission from magnesium and iron ions high in the atmosphere in the aftermath of the meteor shower. Not even the most intense meteor storms on Earth have produced as strong a response as this one. The emission dominated Mars' ultraviolet spectrum for several hours after the encounter and then dissipated over the next two days.

MAVEN also was able to directly sample and determine the composition of some of the comet dust in Mars’ atmosphere. Analysis of these samples by the spacecraft’s Neutral Gas and Ion Mass Spectrometer detected eight different types of metal ions, including sodium, magnesium and iron. These are the first direct measurements of the composition of dust from an Oort Cloud comet. The Oort Cloud, well beyond the outer-most planets that surround our sun, is a spherical region of icy objects believed to be material left over from the formation of the solar system.

Elsewhere above Mars, a joint U.S. and Italian instrument on Mars Express observed a huge increase in the density of electrons following the comet's close approach. This instrument, the Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS), saw a huge jump in the electron density in the ionosphere a few hours after the comet rendezvous. This spike occurred at a substantially lower altitude than the normal density peak in the Martian ionosphere. The increased ionization, like the effects observed by MAVEN, appears to be the result of fine particles from the comet burning up in the atmosphere.

MRO’s Shallow Subsurface Radar (SHARAD) also detected the enhanced ionosphere. Images from the instrument were smeared by the passage of the radar signals through the temporary ion layer created by the comet's dust. SHARAD scientists used this smearing to determine that the electron density of the ionosphere on the planet's night side, where the observations were made, was five to 10 times higher than usual.

Studies of the comet itself, made with MRO's High Resolution Imaging Science Experiment (HiRISE) camera, revealed the nucleus is smaller than the expected 1.2 miles (2 kilometers). The HiRISE images also indicate a rotation period for the nucleus of eight hours, which is consistent with recent preliminary observations by NASA’s Hubble Space Telescope.

MRO’s Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) also observed the comet to see whether signs of any particular chemical constituents stood out in its spectrum. Team members said the spectrum appears to show a dusty comet with no strong emission lines at their instrument’s sensitivity.

In addition to these immediate effects, MAVEN and the other missions will continue to look for long-term perturbations to Mars’ atmosphere.

MAVEN's principal investigator is based at the University of Colorado's Laboratory for Atmospheric and Space Physics in Boulder, and NASA's Goddard Space Flight Center in Greenbelt, Maryland, manages the mission. NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, manages the Mars Reconnaissance Orbiter. Mars Express is a project of the European Space Agency; NASA and the Italian Space Agency jointly funded the MARSIS instrument.

Media teleconference visuals

For more information about NASA's Mars missions, visit:

http://www.nasa.gov/mars

NASA

Guillermo Gonzalo Sánchez Achutegui