NASA : Hubble Captures Brilliant Star Death in “Rotten Egg” Nebula .- Telescopio Espacial Hubble capta la muerte de la estrella brillante en la nebulosa del "huevo podrido"

https://www.nasa.gov/image-feature/goddard/2017/hubble-captures-brilliant-star-death-in-rotten-egg-nebula

The Calabash Nebula, pictured here — which has the technical name OH 231.8+04.2 — is a spectacular example of the death of a low-mass star like the sun. This image taken by the NASA/ESA Hubble Space Telescope shows the star going through a rapid transformation from a red giant to a planetary nebula, during which it blows its outer layers of gas and dust out into the surrounding space. The recently ejected material is spat out in opposite directions with immense speed — the gas shown in yellow is moving close to one million kilometers per hour (621,371 miles per hour).

Astronomers rarely capture a star in this phase of its evolution because it occurs within the blink of an eye — in astronomical terms. Over the next thousand years the nebula is expected to evolve into a fully-fledged planetary nebula.

The nebula is also known as the Rotten Egg Nebula because it contains a lot of sulphur, an element that, when combined with other elements, smells like a rotten egg — but luckily, it resides over 5,000 light-years away in the constellation of Puppis.

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Image credit: ESA/Hubble & NASA, Acknowledgement: Judy Schmidt
Text credit: European Space Agency

Last Updated: Feb. 3, 2017

Editor: Karl Hille

Tags:  Goddard Space Flight Center, Hubble Space Telescope, Image of the Day, Nebulae, Stars, Supernova,

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Guillermo Gonzalo Sánchez Achutegui
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NASA : NASA's K2 mission: The Kepler Space Telescope's Second Chance to Shine.- misión de la NASA K2: la segunda oportunidad del telescopio espacial Kepler de brillar

Hola amigos: A VUELO DE UN QUINDE EL BLOG., hemos recibido información de la Agencia Espacial NASA, los trabajos que está haciendo al Telescopio Espacial Kepler en la investigación de detectar algún exoplaneta que reúna las características de La Tierra: que pueda tener vida, las investigadores espaciales tienen esperanzas que la Misión Kepker2.....

Los ingenieros apiñados en torno a una pantalla de telemetría, y el ambiente era tenso. Estaban viendo flujos de datos desde una nave espacial paralizado más de 50 millones de millas de distancia - tan lejos que incluso a la velocidad de la luz, se tardó casi nueve minutos para una señal viaje a la nave espacial y atrás.

La NASA, piensa que:

Los descubrimientos en rollo

Un poco más de dos años después del momento de tensión para los ingenieros de bolas, K2 ha cumplido su promesa con una amplitud de descubrimientos. Continuando con el legado exoplaneta-caza, K2 ha descubierto más de tres docenas de exoplanetas y con más de 250 candidatos en espera de confirmación. Un puñado de estos mundos son estrellas cercano a la Tierra y la órbita de tamaño que son brillantes y relativamente cercanas en comparación con los descubrimientos de Kepler, permitiendo a los científicos para llevar a cabo estudios de seguimiento. De hecho, estos exoplanetas son probables objetivos futuros para el telescopio espacial Hubble y el próximo telescopio espacial James Webb (JWST), con la posibilidad de estudiar las atmósferas de estos planetas en busca de firmas indicativos de la vida.

Mas información

More information.....

http://www.nasa.gov/feature/ames/nasas-k2-mission-the-kepler-space-telescopes-second-chance-to-shine

The engineers huddled around a telemetry screen, and the mood was tense. They were watching streams of data from a crippled spacecraft more than 50 million miles away – so far that even at the speed of light, it took nearly nine minutes for a signal to travel to the spacecraft and back.

Engineers developed an innovative way to stabilize and control the spacecraft. This technique of using the sun as the "third wheel" has Kepler searching for planets again, but also making discoveries on young stars to supernovae.

Credits: NASA Ames/W Stenzel

Kepler's Second Light: How K2 Works

 

It was late August 2013, and the group of about five employees at Ball Aerospace in Boulder, Colorado, was waiting for NASA’s Kepler space telescope to reveal whether it would live or die. A severe malfunction had robbed the planet-hunting Kepler of its ability to stay pointed at a target without drifting off course.

The engineers had devised a remarkable solution: using the pressure of sunlight to stabilize the spacecraft so it could continue to do science. Now, there was nothing more they could do but wait for the spacecraft to reveal its fate.

“You’re not watching it unfold in real time,” said Dustin Putnam, Ball’s attitude control lead for Kepler. “You’re watching it as it unfolded a few minutes ago, because of the time the data takes to get back from the spacecraft.”

Finally, the team received the confirmation from the spacecraft they had been waiting for. The room broke out in cheers. The fix worked! Kepler, with a new lease on life, was given a new mission as K2. But the biggest surprise was yet to come. A space telescope with a distinguished history of discovering distant exoplanets – planets orbiting other stars – was about to outdo even itself, racking up hundreds more discoveries and helping to usher in entirely new opportunities in astrophysics research.

“Many of us believed that the spacecraft would be saved, but this was perhaps more blind faith than insight,” said Tom Barclay, senior research scientist and director of the Kepler and K2 guest observer office at NASA’s Ames Research Center in California's Silicon Valley. "The Ball team devised an ingenious solution allowing the Kepler space telescope to shine again."

The discoveries roll in

A little more than two years after the tense moment for the Ball engineers, K2 has delivered on its promise with a breadth of discoveries. Continuing the exoplanet-hunting legacy, K2 has discovered more than three dozen exoplanets and with more than 250 candidates awaiting confirmation. A handful of these worlds are near-Earth-sized and orbit stars that are bright and relatively nearby compared with Kepler discoveries, allowing scientists to perform follow-up studies. In fact, these exoplanets are likely future targets for the Hubble Space Telescope and the forthcoming James Webb Space Telescope (JWST), with the potential to study these planets’ atmospheres in search of signatures indicative of life.

 

In this artist’s conception, a tiny rocky object vaporizes as it orbits a white dwarf star. Astronomers have detected the first planetary object transiting a white dwarf using data from the K2 mission. Slowly the object will disintegrate, leaving a dusting of metals on the surface of the star.

Credits: CfA/Mark A. Garlick

Dead star devours mini-planet

K2 also has astronomers rethinking long-held planetary formation theory, and the commonly understood lonely "hot Jupiter" paradigm. The unexpected discovery of a star with a close-in Jupiter-sized planet sandwiched between two smaller companion planets now has theorists back at their computers reworking the models, and has sent astronomers back to their telescopes in search of other hot Jupiter companions.

“It remains a mystery how a giant planet can form far out and migrate inward leaving havoc in its wake and still have nearby planetary companions,” said Barclay.

Like its predecessor, K2 searches for planetary transits – the tiny, telltale dip in the brightness of a star as a planet crosses in front – and for the first time caught the rubble from a destroyed exoplanet transiting across the remains of a dead star known as a white dwarf. Exoplanets have long been thought to orbit these remnant stars, but not until K2 has the theory been confirmed.

K2 has fixed its gaze on regions of the sky with densely packed clusters of stars which has revealed the first transiting exoplanet in such an area, popularly known as the Hyades star cluster. Clusters are exciting places to find exoplanets because stars in a cluster all form around the same time, giving them all the same "born-on" date. This helps scientists understand the evolution of planetary systems.

 

Seventy days worth of solar system observations from K2 are highlighted in this sped-up movie. Neptune, in a dance with its moons, demonstrates the solar system in action. Neptune appears on day 15, followed by its moon Triton, which looks small and faint. Keen-eyed observers can also spot Neptune's tiny moon Nereid at day 24.

Credits: NASA/Ames/SETI/J. Rowe

VIDEO: Neptune Dances with Its Moons

 

The repurposed spacecraft boasts discoveries beyond the realm of exoplanets. Mature stars – about the age of our sun and older – largely populated the original single Kepler field of view. In contrast, many K2 fields see stars still in the process of forming. In these early days, planets also are assembled and by looking at the timescales of star formation, scientists gain insight into how our own planet formed.

Studies of one star-forming region, called Upper Scorpius, compared the size of young stars observed by K2 with computational models. The result demonstrated fundamental imperfections in the models. While the reason for these discrepancies is still under debate, it likely shows that magnetic fields in stars do not arise as researchers expect.

Looking in the ecliptic – the orbital path traveled around the sun by the planets of our solar system and the location of the zodiac – K2 also is well equipped to observe small bodies within our own solar system such as comets, asteroids, dwarf planets, ice giants and moons. Last year, for instance, K2 observed Neptune in a dance with its two moons, Triton and Nereid. This was followed by observations of Pluto and Uranus.

“K2 can’t help but observe the dynamics of our planetary system, " said Barclay. "We all know that planets follow laws of motion but with K2 we can see it happen.”

These initial accomplishments have come in the first year and a half since K2 began in May 2014, and have been carried off without a hitch. The spacecraft continues to perform nominally.

Searching for far out worlds

In April, K2 will take part in a global experiment in exoplanet observation with a special observing period or campaign, Campaign 9. In this campaign, both K2 and astronomers at ground-based observatories on five continents will simultaneously monitor the same region of sky towards the center of our galaxy to search for small planets, such as the size of Earth, orbiting very far from their host star or, in some cases, orbiting no star at all.

For this experiment, scientists will use gravitational microlensing – the phenomenon that occurs when the gravity of a foreground object, such as a planet, focuses and magnifies the light from a distant background star. This detection method will allow scientists to find and determine the mass of planets that orbit at great distances, like Jupiter and Neptune do our sun.

 

At the first K2 Science Conference in Nov. 2015, nearly 200 scientists from around the world convened to discuss their research using K2 data. Knicole Colon, K2 support scientist, walks through the K2 observing opportunities available to the science community. To date, nearly 800 scientists have authored more than 100 scientific papers using K2 data.

Credits: Michele Johnson/NASA Ames

 

Design by community

What could turn out to be one of the most important legacies of K2 has little to do with the mechanics of the telescope, now operating on two wheels and with an assist from the sun.

The Kepler mission was organized along traditional lines of scientific discovery: a targeted set of objectives carefully chosen by the science team to answer a specific question on behalf of NASA – how common or rare are "Earths" around other suns?

K2’s modified mission involves a whole new approach-- engaging the scientific community at large and opening up the spacecraft's capabilities to a broader audience.

"The new approach of letting the community decide the most compelling science targets we’re going to look at has been one of the most exciting aspects," said Steve Howell, the Kepler and K2 project scientist at Ames. "Because of that, the breadth of our science is vast, including star clusters, young stars, supernovae, white dwarfs, very bright stars, active galaxies and, of course, exoplanets.”

In the new paradigm, the K2 team laid out some broad scientific objectives for the mission and planned to operate the spacecraft on behalf of the community. 

Kepler’s field of view surveyed just one patch of sky in the northern hemisphere. The K2 ecliptic field of view provides greater opportunities for Earth-based observatories in both the northern and southern hemispheres, allowing the whole world to participate.

With more than two years of fuel remaining, the spacecraft’s scientific future continues to look unexpectedly bright.

Ames manages the Kepler and K2 missions for NASA’s Science Mission Directorate. NASA's Jet Propulsion Laboratory in Pasadena, California, managed Kepler mission development. Ball Aerospace & Technologies Corporation operates the flight system with support from the Laboratory for Atmospheric and Space Physics at the University of Colorado in Boulder.

For more information about the Kepler and K2 missions, visit:

http://www.nasa.gov/kepler

Authored by Michele Johnson and H. Pat Brennan/JPL

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Media contact: 

Michele Johnson
Ames Research Center, Moffett Field, Calif.
650-604-6982
michele.johnson@nasa.gov

Last Updated: March 9, 2016

Editor: Michele Johnson

Tags:  Ames Research Center, Distant Planets, Kepler and K2, Neptune, Stars, Supernova, Universe,

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Guillermo Gonzalo Sánchez Achutegui

ayabaca@gmail.com

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NASA : Supernova SN 2014J Explodes

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Supernova SN 2014J Explodes

New data from NASA’s Chandra X-ray Observatory has provided stringent constraints on the environment around one of the closest supernovas discovered in decades. The Chandra results provide insight into possible cause of the explosion, as described in our press release.

On January 21, 2014, astronomers witnessed a supernova soon after it exploded in the Messier 82, or M82, galaxy. Telescopes across the globe and in space turned their attention to study this newly exploded star, including Chandra.  Astronomers determined that this supernova, dubbed SN 2014J, belongs to a class of explosions called “Type Ia” supernovas. These supernovas are used as cosmic distance-markers and played a key role in the discovery of the Universe’s accelerated expansion, which has been attributed to the effects of dark energy.  Scientists think that all Type Ia supernovas involve the detonation of a white dwarf. One important question is whether the fuse on the explosion is lit when the white dwarf pulls too much material from a companion star like the Sun, or when two white dwarf stars merge.

This image contains Chandra data, where low, medium, and high-energy X-rays are red, green, and blue respectively. The boxes in the bottom of the image show close-up views of the region around the supernova in data taken prior to the explosion (left), as well as data gathered on February 3, 2014, after the supernova went off (right).  The lack  of the detection of X-rays detected by Chandra is an important clue for astronomers looking for the exact mechanism of how this star exploded.

The non-detection of X-rays reveals that the region around the site of the supernova explosion is relatively devoid of material. This finding is a critical clue to the origin of the explosion. Astronomers expect that if a white dwarf exploded because it had been steadily collecting matter from a companion star prior to exploding, the mass transfer process would not be 100% efficient, and the white dwarf would be immersed in a cloud of gas.

If a significant amount of material were surrounding the doomed star, the blast wave generated by the supernova would have struck it by the time of the Chandra observation, producing a bright X-ray source. Since they do not detect any X-rays, the researchers determined that the region around SN 2014J is exceptionally clean.

A viable candidate for the cause of SN 2014J must explain the relatively gas-free environment around the star prior to the explosion.  One possibility is the merger of two white dwarf stars, in which case there might have been little mass transfer and pollution of the environment before the explosion. Another is that several smaller eruptions on the surface of the white dwarf cleared the region prior to the supernova.  Further observations a few hundred days after the explosion could shed light on the amount of gas in a larger volume, and help decide between these and other scenarios.

A paper describing these results was published in the July 20 issue of The Astrophysical Journal and is available online. The first author is Raffaella Margutti from the Harvard-Smithsonian Center for Astrophysics (CfA) in Cambridge, MA, and the co-authors are Jerod Parrent (CfA), Atish Kamble (CfA), Alicia Soderberg (CfA), Ryan Foley (University of Illinois at Urbana-Champaign), Dan Milisavljevic (CfA), Maria Drout (CfA), and Robert Kirshner (CfA).

Image Credit: NASA/CXC/SAO/R.Margutti et al

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NASA’s Chandra Observatory Searches for Trigger of Nearby Supernova

NASA’s Chandra X-ray Observatory is helping determine what caused SN 2014J, one of the closest supernovas discovered in decades. By comparing X-ray data taken before and after the stellar explosion, scientists can learn more about what set it off.

Image Credit: 

NASA/SAO/CXC/R. Margutti et al

 

New data from NASA’s Chandra X-ray Observatory offer a glimpse into the environment of a star before it exploded earlier this year, and insight into what triggered one of the closest supernovas witnessed in decades.
The data gathered on the Jan. 21 explosion, a Type Ia supernova, allowed scientists to rule out one possible cause. These supernovas may be triggered when a white dwarf takes on too much mass from its companion star, immersing it in a cloud of gas that produces a significant source of X-rays after the explosion.
Astronomers used NASA's Swift and Chandra telescopes to search the nearby Messier 82 galaxy, the location of the explosion, for such an X-ray source. However, no source was found, revealing the region around the site of the supernova is relatively devoid of material.
“While it may sound a bit odd, we actually learned a great deal about this supernova by detecting absolutely nothing,” said Raffaella Margutti of the Harvard-Smithsonian Center for Astrophysics (CfA) in Cambridge, Massachusetts, who led the study. “Now we can essentially rule out that the explosion was caused by a white dwarf continuously pulling material from a companion star.”
This supernova, SN 2014J, could instead have been caused by the merger of two white dwarf stars, an event that should result in little or no X-rays after the explosion. Further observations could rule out or confirm other possible triggers.
“Being able to eliminate one of the main possible explanations for what caused SN 2014J to explode is a big step,” said CfA’s Atish Kamble, a co-author of the study. “The next step is to narrow things down even further.”
Type Ia supernovas are used as cosmic distance-markers, and have played a key role in the discovery of the universe’s accelerated expansion. At about 12 million light-years from Earth, SN 2014J and its host galaxy are close -- from a cosmic perspective. This offers scientists a chance to observe details that would be too hard to detect in more distant supernovas.
“It’s crucial that we understand exactly how these stars explode because so much is riding on our observations of them for cosmology,” said co-author Jerod Parrent also from CfA. “SN 2014J might be a chance of a lifetime to study one of these supernovas in detail as it happens.”
The study of SN 2014J is similar to a study led by Margutti about another supernova, SN 2011fe, in the nearby galaxy M101.
This study was conducted by CfA’s Supernova Forensics Team, led by Alicia Soderberg. The results were published online and in the July 20 print issue of The Astrophysical Journal.
NASA's Marshall Space Flight Center in Huntsville, Alabama, manages the Chandra program for NASA's Science Mission Directorate in Washington. The Smithsonian Astrophysical Observatory in Cambridge, Massachusetts, controls Chandra's science and flight operations.
For an additional interactive image, podcast, and video on the findings, visit:

http://chandra.si.edu

For a preprint of the study results in The Astrophysical Journal, visit:

http://arxiv.org/abs/1405.1488

For Chandra images, multimedia and related materials, visit:

http://www.nasa.gov/chandra

 

NASA

Guillermo Gonzalo Sánchez Achutegui

ayabaca@gmail.com

ayabaca@hotmail.com

ayabaca@yahoo.com

NASA : Hardy Star Survives Supernova Blast

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Hardy Star Survives Supernova Blast

When a massive star runs out fuel, it collapses and explodes as a supernova. Although these explosions are extremely powerful, it is possible for a companion star to endure the blast. A team of astronomers using NASA’s Chandra X-ray Observatory and other telescopes has found evidence for one of these survivors.

This hardy star is in a stellar explosion’s debris field − also called its supernova remnant − located in an HII region called DEM L241. An HII (pronounced "H-two") region is created when the radiation from hot, young stars strips away the electrons from neutral hydrogen atoms (HI) to form clouds of ionized hydrogen (HII). This HII region is located in the Large Magellanic Cloud, a small companion galaxy to the Milky Way.

A new composite image of DEM L241 contains Chandra data (purple) that outlines the supernova remnant. The remnant remains hot and therefore X-ray bright for thousands of years after the original explosion occurred. Also included in this image are optical data from the Magellanic Cloud Emission Line Survey (MCELS) taken from ground-based telescopes in Chile (yellow and cyan), which trace the HII emission produced by DEM L241. Additional optical data from the Digitized Sky Survey (white) are also included, showing stars in the field.

R. Davies, K. Elliott, and J. Meaburn, whose last initials were combined to give the object the first half of its name, first mapped DEM L241 in 1976. The recent data from Chandra revealed the presence of a point-like X-ray source at the same location as a young massive star within DEM L241’s supernova remnant.

Astronomers can look at the details of the Chandra data to glean important clues about the nature of X-ray sources. For example, how bright the X-rays are, how they change over time, and how they are distributed across the range of energy that Chandra observes.

In this case, the data suggest that the point-like source is one component of a binary star system. In such a celestial pair, either a neutron star or black hole (formed when the star went supernova) is in orbit with a star much larger than our Sun. As they orbit one another, the dense neutron star or black hole pulls material away its companion star through the wind of particles that flows away from its surface. If this result is confirmed, DEM L241 would be only the third binary containing both a massive star and a neutron star or black hole ever found in the aftermath of a supernova.

Chandra’s X-ray data also show that the inside of the supernova remnant is enriched in oxygen, neon and magnesium. This enrichment and the presence of the massive star imply that the star that exploded had a mass greater than 25 times, to perhaps up to 40 times, that of the Sun.

Optical observations with the South African Astronomical Observatory's 1.9-meter telescope show the velocity of the massive star is changing and that it orbits around the neutron star or black hole with a period of tens of days. A detailed measurement of the velocity variation of the massive companion star should provide a definitive test of whether or not the binary contains a black hole.

Indirect evidence already exists that other supernova remnants were formed by the collapse of a star to form a black hole. However, if the collapsed star in DEM L241 turns out to be a black hole, it would provide the strongest evidence yet for such a catastrophic event.

What does the future hold for this system? If the latest thinking is correct, the surviving massive star will be destroyed in a supernova explosion some millions of years from now. When it does, it may form a binary system containing two neutron stars or a neutron star and a black hole, or even a system with two black holes.

A paper describing these results is available online and was published in the November 10, 2012 issue of The Astrophysical Journal (http://arxiv.org/abs/1208.1453). The authors are Fred Seward of the Harvard-Smithsonian Center for Astrophysics in Cambridge, MA; P. Charles from University of Southampton, UK; D. Foster from the South African Astronomical Observatory in Cape Town, South Africa; J. Dickel and P. Romero from University of New Mexico in Albuquerque, NM; Z. Edwards, M. Perry and R. Williams from Columbus State University in Columbus, GA.

NASA's Marshall Space Flight Center in Huntsville, Ala., manages the Chandra program for NASA's Science Mission Directorate in Washington. The Smithsonian Astrophysical Observatory in Cambridge, Mass., controls Chandra's science and flight operations.

Image credit: X-ray: NASA/CXC/SAO/F. Seward et al; Optical: NOAO/CTIO/MCELS, DSS

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NASA : Supernova Blast Provides Clues to Determining Age of Binary Star System

Image of Circinus X-1, an X-ray binary star system, taken by the Chandra X-ray Observatory. (Credit: NASA)

Data from Supernova Blast Provides Clues to Determining Age of Binary Star Systemhas revealed faint remnants of a supernova explosion and helped researchers determine Circinus X-1 -- an X-ray binary -- is the youngest of this class of astronomical objects found to date.

As the name suggests, X-ray binaries are star systems made up of two parts: a compact stellar remnant -- either a neutron star or a black hole; and a companion star -- a normal star like our sun. As they orbit one another, the neutron star or black hole pulls in gas from the companion star. This heats the gas to millions of degrees, producing intense X-ray radiation and making these star systems some of the brightest X-ray sources in the sky.

Sebastian Heinz and his team at the University of Wisconsin-Madison (UW) discovered Circinus X-1 is less than 4,600 years old, making it the youngest X-ray binary system ever seen. This discovery, made in parallel with a radio telescope in Australia, provides scientists unique insight into the formation of neutron stars and supernovas, and the effect of the supernova's explosion on a nearby companion star.

"X-ray binaries provide us with opportunities to study matter under extreme conditions that would be impossible to recreate in a laboratory," Heinz said. "For the first time, we can study a newly minted neutron star in an X-ray binary system."

Astronomers have detected hundreds of X-ray binaries throughout the Milky Way and other nearby galaxies. However, these older X-ray binaries, with ages typically measured in millions of years, only reveal information about what happens much later in the evolution of these systems.

"It's critical that we see what these X-ray binaries are doing at all stages of their lives," said co-author Paul Sell, also of UW. "Circinus X-1 is showing us what happens in a cosmic blink of an eye after one of these objects is born."

To determine the age of Circinus X-1, the team of astronomers needed to examine the material around the orbiting pair of stars. However, the overwhelming brightness of the neutron star made it too difficult for researchers to observe that interstellar gas. The team recently caught a break, when they observed the neutron star in a very faint state -- dim enough for scientists to detect the X-rays from the supernova shock wave that plowed through the surrounding interstellar gas.

"Since the supernova was triggered by the formation of the neutron star, our limit on the age of the supernova remnant also limits the age of the neutron star in Circinus X-1," said co-author Robert Fender of the University of Oxford in the U.K.

The youth of Circinus X-1 helps explain its wild swings in brightness and the highly unusual orbit of its two stars, which had puzzled astronomers for years. The orbit is very eccentric -- non-circular -- and the period during which the two stars orbit each other is decreasing by several minutes every year. This is exactly what is expected for a young X-ray binary disrupted by a supernova explosion before the gravitational pull of the stars on each other has had time to circularize and stabilize the orbit.

Previous observations with other telescopes indicated the magnetic field of the neutron star in Circinus X-1 is weak. That, in addition to the star system's young age, has led to two possible theories: either a neutron star can be born with a weak magnetic field, or it can quickly become de-magnetized as it pulls material from its companion star onto itself. Neither conclusion was expected from existing theories of neutron star evolution.

In our galaxy, the only other established X-ray binary within a supernova remnant is SS 433, which is between 10,000 and 100,000 years old, and behaves in many ways like an older version of Circinus X-1. Two other candidate X-ray binaries in nearby galaxies have ages similar to SS 433.

In addition to the Chandra data, radio observations from the Australia Telescope Compact Array were critical in these findings. A paper describing these results is available online and appears in the Dec. 3 issue of The Astrophysical Journal.

NASA's Marshall Space Flight Center in Huntsville, Ala., manages the Chandra program for NASA's Science Mission Directorate in Washington. The Smithsonian Astrophysical Observatory in Cambridge, Mass., controls Chandra's science and flight operations.

For more information about Chandra, visit:

http://www.nasa.gov/chandra

and

http://chandra.si.edu

NASA:
Guillermo Gonzalo Sánchez Achutegui
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NASA : 3C 397: An Unusual Galactic Supernova Remnant

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3C 397: An Unusual Galactic Supernova Remnant

3C 397 (also known as G41.1-0.3) is a Galactic supernova remnant with an unusual shape. Researchers think its box-like appearance is produced as the heated remains of the exploded star -- detected by Chandra in X-rays (purple) -- runs into cooler gas surrounding it. This composite of the area around 3C 397 also contains infrared emission from Spitzer (yellow) and optical data from the Digitized Sky Survey (red, green, and blue).

Image credit: X-ray: NASA/CXC/Univ of Manitoba/S.Safi-Harb et al, Optical: DSS, Infrared: NASA/JPL-Caltech

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NASA - Neutron Star Undergoes Wild Behavior Changes

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Neutron Star Undergoes Wild Behavior Changes

These two images from NASA's Chandra X-ray Observatory show a large change in X-ray brightness of a rapidly rotating neutron star, or pulsar, between 2006 and 2013. The neutron star − the extremely dense remnant left behind by a supernova − is in a tight orbit around a low mass star. This binary star system, IGR J18245-2452 is a member of the globular cluster M28.

As described in a press release from the European Space Agency, IGR J18245-2452 provides important information about the evolution of pulsars in binary systems. Pulses of radio waves have been observed from the neutron star as it makes a complete rotation every 3.93 milliseconds (an astonishing rate of 254 times every second), identifying it as a "millisecond pulsar."

The widely accepted model for the evolution of these objects is that matter is pulled from the companion star onto the surface of the neutron star via a disk surrounding it. During this so-called accretion phase, the system is described as a low-mass X-ray binary because bright X-ray emission from the disk is observed. Spinning material in the disk falls onto the neutron star, increasing its rotation rate. The transfer of matter eventually slows down and the remaining material is swept away by the whirling magnetic field of the neutron star as a millisecond radio pulsar forms.

The complete evolution of a low-mass X-ray binary into a millisecond pulsar should happen over several billion years, but in the course of this evolution, the system might switch rapidly between these two states. The source IGR J18245-2452 provides the first direct evidence for such drastic changes in behavior. In observations from July 2002 to May 2013 there are periods when it acts like an X-ray binary and the radio pulses disappear, and there are times when it switches off as an X-ray binary and the radio pulses turn on.

The latest observations with both X-ray and radio telescopes show that the transitions between an X-ray binary and a radio pulsar can take place in both directions and on a time scale that is shorter than expected, maybe only a few days. They also provide powerful evidence for an evolutionary link between X-ray binaries and radio millisecond pulsars.

The X-ray observations contained data from Chandra, ESA's XMM-Newton, the International Gamma-Ray Astrophysics Laboratory (INTEGRAL) and NASA's Swift/XRT and the radio observations used the Australia Telescope Compact Array, the Green Bank Telescope, Parkes radio telescope and the Westerbok Synthesis Radio Telescope.

The observations of IGR J18245-2452 and their implications are described in a paper published in the September 26th, 2013 issue of Nature. The first author is Alessandro Papitto from the Institute of Space Sciences in Barcelona, Spain. The co-authors are C. Ferrigno and E. Bozzo from Universite´ de Gene`ve, Versoix, Switzerland; N. Rea from the Institute of Space Sciences in Barcelona, Spain; L. Pavan from Universite´ de Gene`ve, Versoix, Switzerland; L. Burderi from Universit´a di Cagliari, Monserrato, Italy; M. Burgay from INAF-Osservatorio Astronomico di Cagliari, Capoterra, Italy; S. Campana from INAF-Osservatorio Astronomico di Brera, Lecco, Italy; T. Di Salvo from Universit´a di Palermo, Palermo, Italy; M. Falanga from International Space Science Institute, Bern, Switzerland; M. Filipovi´c from University of Western Sydney, Penrith, Australia; P. Freire from Max-Planck-Institut f´ur Radioastronomie, Bonn, Germany; J. Hessels from Netherlands Institute for Radio Astronomy, Dwingeloo, The Netherlands; A. Possenti from INAF-Osservatorio Astronomico di Cagliari, Capoterra, Italy; S. Ransom from National Radio Astronomy Observatory, Charlottesville, VA; A. Riggio from Universit´a di Cagliari, Monserrato, Italy; P. Romano from INAF-Istituto di Astrosica Spaziale e Fisica Cosmica, Palermo, Italy; J. Sarkissian from CSIRO Astronomy and Space Science, Epping, Australia; I. Stairs from University of British Columbia, Vancouver, Canada; L. Stella from INAF-Osservatorio Astronomico di Roma, Roma, Italy; D. Torres from the Institute of Space Sciences in Barcelona, Spain; M. Wieringa from CSIRO Astronomy and Space Science, Narrabri, Australia and G. Wong from University of Western Sydney, Penrith, Australia.

NASA's Marshall Space Flight Center in Huntsville, Ala., manages the Chandra Program for NASA's Science Mission Directorate in Washington. The Smithsonian Astrophysical Observatory controls Chandra's science and flight operations from Cambridge, Mass.

Image credit: X-ray: NASA/CXC/ICE/A. Papitto et al.

› View large image
› Chandra on Flickr

NASA

Guillermo Gonzalo Sánchez Achutegui

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Astronomía: Nueva imagen de la Nebulosa del Lápiz ¿Una escoba de bruja en el espacio?

Hola amigos: A VUELO DE UN QUINDE EL BLOG., Esta es una nueva imagen de la Nebulosa del Lápiz, obtenida desde el Observatorio La Silla, en Chile. Esta peculiar nube de gas brillante forma parte de un inmenso anillo de escombros, resultantes de una explosión de supernova que tuvo lugar hace unos 11.000 años. La detallada imagen ha sido captada por la cámara Wide Field Imager, instalada en el telescopio MPG/ESO de 2,2 metros

 La Nebulosa del Lápiz, los extraños restos de una vasta explosión

La Nebulosa del Lápiz, (NGC 2736) con su extraña forma, puede verse en esta imagen del Observatorio La Silla de ESO, en Chile. Esta nebulosa es una pequeña parte de un gran remanente dejado por una explosión de supernova que tuvo lugar hace unos  11.000 años. La imagen fue obtenida por la cámara Wide Field Imager, instalada en el telescopio MPG/ESO de 2,2 metros, en el Observatorio La Silla de ESO, en Chile.

Crédito: ESO

La Nebulosa del Lápiz, en la constelación austral de La Vela

Este mapa muestra la ubicación de la Nebulosa del Lápiz (NGC 2736) en la Constelación de La Vela. La mayor parte de las estrellas de este mapa pueden verse a simple vista bajo buenas condiciones meteorológicas, y se ha destacado la ubicación de la Nebulosa de Lápiz con un círculo rojo. Esta débil nebulosa requiere de un cielo oscuro y de potentes telescopios para hacerla visible como una larga raya oscura.

Crédito: ESO, IAU and Sky & Telescope

Visión de amplio campo del cielo que rodea a la Nebulosa del Lápiz

Esta imagen de la región del cielo que rodea a la Nebulosa del Lápiz muestra un paisaje celeste espectacular, protagonizado por los filamentos azules de los remanentes de la supernova Vela, el brillo rojizo de las nubes de hidrógeno e incontables estrellas. Es una composición de color hecha con exposiciones del sondeo Digitized Sky Survey 2.
Crédito:
ESO/Digitized Sky Survey 2
Acknowledgment: Davide De Martin.
 

Pese a la aparente calma y la belleza estática de una noche estrellada, el Universo está lejos de ser un lugar tranquilo. Las estrellas nacen y mueren en un ciclo sin fin, y algunas veces la muerte de una estrella puede dar lugar a imágenes de belleza sin igual en las que el material es expulsado al espacio formando extrañas estructuras en el cielo.

Esta nueva imagen del instrumento Wide Field Imager, instalado en el telescopio de ESO MPG/ESO de 2,2 metros, ubicado en el Observatorio La Silla, en Chile, muestra la Nebulosa del Lápiz [1] que destaca sobre un rico fondo estrellado. Esta nube de extraña forma, también conocida como NGC 2736, es una pequeña parte de un remanente de una supernova [2] situada en la constelación austral de La Vela. Estos brillantes filamentos fueron generados por la violenta muerte de una estrella que tuvo lugar hace unos 11.000 años. Las partes más brillantes tienen forma de lápiz, de ahí el nombre, pero la estructura completa se asemeja más a una típica escoba de bruja.

El remanente de la supernova de la Constelación de La Vela es una masa de gas en expansión originada por la explosión. Inicialmente, la onda de choque se movía a millones de kilómetros por hora, pero a medida que se expandía a través del espacio fue perforando el gas entre las estrellas, frenándola considerablemente y generando extrañas nebulosas de retorcidas formas. La Nebulosa de Lápiz es la parte más brillante de esta enorme estructura.

Esta nueva imagen muestra inmensas y tenues estructuras filamentosas, nudos de gas más pequeños y grupos de gas difuso. La apariencia luminosa de la nebulosa proviene de las densas regiones de gas que han sido impulsadas por la onda de choque de la supernova. Dado que la onda de choque viaja a través del espacio, atraviesa la materia interestelar. Al principio, el gas se calentó en millones de grados, pero posteriormente se enfrió y aún emite un débil brillo, captado en la nueva imagen.

Estudiando los diferentes colores de la nebulosa, los astrónomos han podido conocer la temperatura del gas. Algunas regiones aún están tan calientes que la emisión está dominada por átomos de oxígeno ionizado, que en esta imagen podemos ver brillando en tonos azules. Otras regiones más frías pueden verse en tonos rojizos, debido a la emisión del hidrógeno.

La Nebulosa del Lápiz mide unos 0,75 años luz y se mueve a través del medio interestelar a unos 650.000 kilómetros por hora. Sorprendentemente, pese a que se encuentra a una distancia de unos 800 años luz de la Tierra, esto significa que cambiará notablemente su posición relativa con respecto a las estrellas del fondo a lo largo del tiempo que dura una vida humana. Incluso después de 11.000 años la explosión de supernova sigue cambiando el aspecto del cielo nocturno.

Notas

[1] La Nebulosa del Lápiz, también conocida como NGC 2736, y apodada algunas veces como el “Rayo de Herschel”, fue descubierta por el astrónomo británico John Herschel en 1835 durante una estancia en Sudáfrica. La describió como “un rayo extraordinariamente largo y estrecho de luz excesivamente débil”.

[2] Una supernova es una violenta explosión estelar resultante de la muerte de una estrella masiva o de una enana blanca en un sistema estelar doble. La estructura resultante de la explosión se denomina remanente de supernova. Este consiste en material eyectado que se expande a velocidades supersónicas por el medio interestelar circundante. Las supernovas son la fuente principal de elementos químicos pesados para el medio interestelar, lo que enriquecerá una nueva generación de estrellas y planetas.

Información adicional

El año 2012 marca el 50 aniversario de la creación del Observatorio Europeo Austral (European Southern Observatory, ESO). ESO es la principal organización astronómica intergubernamental de Europa y el observatorio astronómico más productivo del mundo. Quince países apoyan esta institución: Alemania, Austria, Bélgica, Brasil, Dinamarca, España, Finlandia, Francia, Holanda, Italia, Portugal, el Reino Unido, República Checa, Suecia y Suiza. ESO desarrolla un ambicioso programa centrado en el diseño, construcción y operación de poderosas instalaciones de observación terrestres que permiten a los astrónomos hacer importantes descubrimientos científicos. ESO también desarrolla un importante papel al promover y organizar la cooperación en investigación astronómica. ESO opera tres sitios únicos de observación de categoría mundial en Chile: La Silla, Paranal y Chajnantor. En Paranal, ESO opera el Very Large Telescope, el observatorio óptico más avanzado del mundo, y dos telescopios de rastreo. VISTA trabaja en el infrarrojo y es el telescopio de rastreo más grande del mundo, y el VST (sigla en inglés del Telescopio de Rastreo del VLT) es el telescopio más grande diseñado exclusivamente para rastrear el cielo en luz visible. ESO es el socio europeo de un revolucionario telescopio, ALMA, el proyecto astronómico más grande en desarrollo. Actualmente ESO está planificando el European Extremely Large Telescope, E-ELT, el telescopio óptico y de infrarrojo cercano de categoría 40 metros, que llegará a ser “el ojo más grande del mundo para mirar el cielo”.

Enlaces

• Fotos del telescopio MPG/ESO de 2,2 metros
• Otras fotos tomadas con el telescopio MPG/ESO de 2,2 metros
• Fotos de La Silla

Contactos

Francisco Rodríguez
Observatorio Europeo Austral (ESO)
Santiago, Chile
Tlf.: +562 4633019
Correo electrónico: frrodrig@eso.org

Richard Hook
ESO, La Silla, Paranal, E-ELT & Survey Telescopes Press Officer
Garching bei München, Germany
Tlf.: +49 89 3200 6655
Móvil: +49 151 1537 3591
Correo electrónico: rhook@eso.org

Esta es una traducción de la nota de prensa de ESO eso1236.

 ESO

Guillermo Gonzalo sánchez Achutegui

ayabaca@gmail.com

ayabaca@hotmail.com

ayabaca@yahoo.com

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Astronomía: Los restos de una explosión estelar

Hola amigos: A VUELO DE UN QUINDE EL BLOG., El observatorio espacial XMM-Newton de la ESA nos muestra esta semana los restos de una explosión de supernova, el dramático final de una estrella masiva, suspendidos en el tiempo y en el espacio.

Download:

 HI-RES JPEG (Size: 566 kb)

 Composite optical and X-ray picture of supernova remnant G272.2-03.2, taken on 11 December 2001 by ESA’s XMM-Newton. The remnant was discovered in 1994 with ROSAT. The image is 40 x 40 arc minutes.
Credits: XMM-Newton/ESA

 El observatorio espacial XMM-Newton de la ESA nos muestra esta semana los restos de una explosión de supernova, el dramático final de una estrella masiva, suspendidos en el tiempo y en el espacio.

En las longitudes de onda de rayos X, los nudos de gas caliente brillan en tonos verdosos –lo que indica que presentan una temperatura de millones de grados Celsius– llenando la región central del remanente de supernova G272.2-03.2, todavía en expansión.

Un remanente de supernova es la estructura nebulosa que queda cuando una estrella masiva –con una masa de más de ocho veces la de nuestro Sol– agota su reserva de combustible y colapsa sobre sí misma, expulsando sus últimas capas de gas en una explosión cegadora.

En el corazón de la explosión puede quedar una estrella de neutrones o un agujero negro, oculto tras la capa de material compuesta por los restos de la explosión y por el medio interestelar barrido por su onda de choque.

En esta imagen se pueden distinguir dos puntos brillantes cerca del borde derecho del remanente, iluminados por la interacción de las ondas de choque con el medio que las rodea. Estos restos tan sólo tienen unos pocos miles de años – la expansión de la onda de choque tarda cientos de miles de años en frenarse.

Al estudiar los remanentes de supernovas en las longitudes de onda de los rayos X, los astrónomos son capaces de determinar la abundancia y la distribución de los distintos elementos químicos que había forjado la estrella durante las últimas etapas de su vida.

Estos datos pueden aportar nuevas pistas sobre la masa de la estrella original y sobre la dinámica de la explosión.

Las motas azules y blancas que salpican la imagen son objetos estelares que rodean a los restos de la supernova. 

 ESA

Guillermo Gonzalo Sánchez Achutegui

ayabaca@gmail.com

ayabaca@hotmail.com

ayabaca@yahoo.com

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Astronomía: Un remolino azul en El Río

Hola amigos: A VUELO DE UN QUINDE EL BLOG., En esta nueva imagen, obtenida con el telescopio VLT (Very Large Telescope) de ESO, vemos la galaxia NGC 1187. Esta impresionante espiral se encuentra a unos 60 millones de años luz de nosotros, en la constelación de Eridanus (El Río). NGC 1187 ha albergado dos explosiones de supernova durante los últimos treinta años, la última en el año 2007. Esta imagen de la galaxia es la más precisa de las obtenidas hasta el momento.

 Una tranquila galaxia que alberga fenómenos violentos.

Imagen de la galaxia espiral NGC 1187 obtenida con el VLT

En esta imagen, obtenida con el telescopio VLT (Very Large Telescope) de ESO, vemos la galaxia NGC 1187. Esta impresionante espiral se encuentra a unos 60 millones de años luz de nosotros en la constelación de Eridanus (El Río). NGC 1187 ha albergado dos explosiones de supernova durante los últimos treinta años, la última en el año 2007.

Crédito: ESO

Imagen de la galaxia espiral NGC 1187 obtenida con el VLT (con anotaciones)

En esta imagen, obtenida con el telescopio VLT (Very Large Telescope) de ESO, vemos la galaxia NGC 1187. Esta impresionante espiral se encuentra a unos 60 millones de años luz de nosotros en la constelación de Eridanus (El Río). NGC 1187 ha albergado dos explosiones de supernova durante los últimos treinta años, la última en el año 2007. Esta supernova, enmarcada en un círculo, aún puede verse débilmente en la imagen.

Crédito: ESO

 

La galaxia espiral NGC 1187 en la constelación de Eridanus

Este mapa muestra la ubicación de NGC 1187 en la constelación de Eridanus (El Río). En la imagen, la galaxia NGC 1187 está enmarcada en un círculo rojo. La mayor parte de las estrellas que se muestran en este mapa pueden verse a simple vista bajo buenas condiciones atmosféricas; la propia galaxia puede detectarse como una mancha borrosa si se observa con telescopios de aficionados de tamaño medio.

Crédito:

ESO, IAU and Sky & Telescope

Visión de amplio campo del cielo que rodea a la galaxia espiral NGC 1187

 Esta visión de amplio campo se centra en la galaxia espiral NGC 1187, en la constelación de Eridanus (El Río). Es una composición de color realizada con exposiciones del sondeo Digitized Sky Survey 2 (DSS2). La distorsionada galaxia compañera ESO 480-G020, puede verse en el extreme superior derecho de la galaxia NGC 1187, cerca de una estrella. La brillante estrella del la parte inferior es Tau³ Eridani.

Crédito: ESO/Digitized Sky Survey 2. Acknowledgment: Davide De Martin.

Video:

Acercamiento a la galaxia espiral NGC 1187

http://www.eso.org/public/chile/videos/eso1231a/

Esta secuencia de vídeo comienza con una visión de amplio campo de la gran pero débil constelación de Eridanus (El Río), no muy alejada de la más conocida Orion (El Cazador). A medida que nos acercamos vemos un pequeño parche de luz que se acaba revelando como una atractiva galaxia espiral llamada NGC 1187. La detallada imagen final muestra una nueva imagen de este objeto obtenida por el telescopio VLT.

Crédito:

ESO/A. Fujii/Digitized Sky Survey 2. Acknowledgment: Davide De Martin. Music: Disasterpeace

En esta nueva imagen, obtenida con el telescopio VLT (Very Large Telescope) de ESO, vemos la galaxia NGC 1187. Esta impresionante espiral se encuentra a unos 60 millones de años luz de nosotros, en la constelación de Eridanus (El Río). NGC 1187 ha albergado dos explosiones de supernova durante los últimos treinta años, la última en el año 2007. Esta imagen de la galaxia es la más precisa de las obtenidas hasta el momento.

La galaxia NGC 1187 [1] se ve casi de frente en la nueva imagen del VLT, que nos muestra con claridad su estructura espiral. Pueden verse alrededor de media docena de brazos espirales prominentes, cada uno de los cuales contiene grandes cantidades de gas y polvo. Los rastros azulados de los brazos espirales indican la presencia de estrellas jóvenes nacidas de las nubes de gas interestelar.

Mirando hacia las zonas centrales, vemos cómo brilla el protuberante centro en tonos amarillos. Esta parte de la galaxia está compuesta, principalmente, de estrellas viejas, gas y polvo. En el caso de NGC 1187, más que un centro redondeado, hay una sutil estructura central en forma de barra. Se cree que esta característica forma barrada actúa como un mecanismo que canaliza el gas procedente de los brazos espirales hacia el centro, aumentando la formación estelar en esa zona.

En los alrededores de la galaxia, pueden verse muchas más galaxias más débiles y más distantes. Algunas incluso brillan a través del disco de NGC 1187. Sus tonos predominantemente rojizos contrastan con los cúmulos de estrellas azul pálido de los objetos más cercanos.

NGC 1187 parece una galaxia tranquila e inmutable, pero ha albergado dos explosiones de supernova desde 1982. Una supernova es una violenta explosión estelar, resultante de la muerte de una estrella masiva o de una enana blanca en un sistema binario [2]. Las supernovas son uno de los fenómenos más energéticos del universo, y son tan brillantes que a menudo iluminan brevemente una galaxia al completo antes de desaparecer de nuestra vista durante semanas o meses. Durante este corto periodo de tiempo una supernova puede irradiar tanta energía como la que se estima que emitirá el Sol a lo largo de toda su vida.

En octubre de 1982, se descubrió la primera supernova en NGC 1187 — SN 1982R [3]. Fue desde La Silla, un observatorio de ESO, y más recientemente, en 2007, el astrónomo aficionado Berto Monard, localizó desde Sudáfrica otra supernova en esta galaxia — SN 2007Y. Posteriormente, un equipo de astrónomos elaboró un detallado estudio y monitorizó SN 2007Y durante alrededor de un año utilizando numerosos telescopios [4]. Esta nueva imagen de NGC 1187 fue creada a partir de observaciones obtenidas como parte de este estudio y la supernova puede verse, mucho después de su pico de brillo máximo, cerca del extremo inferior de la imagen.

Estos datos fueron obtenidos utilizando el instrumento FORS1, instalado en el Very Large Telescope de ESO, en el Observatorio Paranal, en Chile.

Notas

[1] Esta galaxia fue descubierta por William Herschel en 1784 desde Inglaterra.

[2] Un tipo de explosión de supernova ocurre al final de la vida de una estrella masiva — estrellas con más de ocho masas solares — cuando el combustible de su núcleo se agota y la estrella ya no es capaz de contrarrestar el colapso gravitatorio, produciendo una violenta explosión. Alternativamente, una explosión de supernova puede también tener lugar en un sistema estelar binario, en el cual una enana blanca (compuestas principalmente de carbono y oxígeno) atrae materia de su estrella compañera, de mayor masa. Si se transfiere la suficiente cantidad de masa, la estrella empezará a colapsar, produciendo una explosión de supernova.

[3] La Unión Astronómica Internacional es responsable de poner nombre a las supernovas tras su descubrimiento. El nombre se compone del año del descubrimiento, seguido por una o dos letras. Las primeras 26 supernovas del año se nombran con letras mayúsculas de la A a la Z. Las supernovas posteriores se designan con dos letras minúsculas.

[4] Pueden encontrar más información sobre SN 2007Y en este artículo de Stritzinger et al.

Información adicional

El año 2012 marca el 50 aniversario de la creación del Observatorio Europeo Austral (European Southern Observatory, ESO). ESO es la principal organización astronómica intergubernamental de Europa y el observatorio astronómico más productivo del mundo. Quince países apoyan esta institución: Alemania, Austria, Bélgica, Brasil, Dinamarca, España, Finlandia, Francia, Holanda, Italia, Portugal, el Reino Unido, República Checa, Suecia y Suiza. ESO desarrolla un ambicioso programa centrado en el diseño, construcción y operación de poderosas instalaciones de observación terrestres que permiten a los astrónomos hacer importantes descubrimientos científicos. ESO también desarrolla un importante papel al promover y organizar la cooperación en investigación astronómica. ESO opera tres sitios únicos de observación de categoría mundial en Chile: La Silla, Paranal y Chajnantor. En Paranal, ESO opera el Very Large Telescope, el observatorio óptico más avanzado del mundo, y dos telescopios de rastreo. VISTA trabaja en el infrarrojo y es el telescopio de rastreo más grande del mundo, y el VST (sigla en inglés del Telescopio de Rastreo del VLT) es el telescopio más grande diseñado exclusivamente para rastrear el cielo en luz visible. ESO es el socio europeo de un revolucionario telescopio, ALMA, el proyecto astronómico más grande en desarrollo. Actualmente ESO está planificando el European Extremely Large Telescope, E-ELT, el telescopio óptico y de infrarrojo cercano de categoría 40 metros, que llegará a ser “el ojo más grande del mundo para mirar el cielo”.

Enlaces

• Fotos del VLT
• Otras imágenes obtenidas con el VLT

 ESO
Guillermo Gonzalo Sánchez Achuteguui
ayabaca@gmail.com
ayabaca@hotmail.com
ayabaca@yahoo.com
 Inscríbete en el Foro del blog y participa : A Vuelo De Un Quinde - El Foro!