Author: Fraser Cain

Image credit: Hubble

Although stars can burn for billions of years, their final stages can take a relatively short period of time. In many cases, it only takes a few hundred thousand years for dying stars to slough off their outer layers to create the familiar planetary nebula. Since they happen so quickly, they’re relatively rare to find, but astronomers think they’ve got a candidate with a relatively nearby star called V Hydra. The star is in its final stages, and jets of material have just begun emanating from it.

It takes only a few hundred to a thousand years for a dying Sun-like star, many billions of years old, to transform into a dazzling, glowing cloud called a planetary nebula. This relative blink in a long lifetime means that a Sun-like star’s final moments – the crucial phase when its planetary nebula takes shape – have, until now, gone undetected.

In research reported in the Nov. 20 issue of Nature, astronomers led by Dr. Raghvendra Sahai of NASA’s Jet Propulsion Laboratory, Pasadena, Calif., have caught one such dying star in the act. This nearby star, called V Hydrae, has been captured by the Space Telescope Imaging Spectrograph onboard NASA’s Hubble Space Telescope in the last stages of its demise, just as material has begun to shoot away from it in a high-speed jet outflow.

While previous studies have indicated the role of jet outflows in shaping planetary nebulae, the new findings represent the first time these jets have been directly detected.

“The discovery of a newly launched jet outflow is likely to have a significant impact on our understanding of this short-lived stage of stellar evolution and will open a window onto the ultimate fate of our Sun,” said Sahai.

Other institutions contributing to this paper include: University of California, Los Angeles; Princeton University, Princeton, New Jersey; Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts; and Valdosta State University, Valdosta, Georgia.

Low-mass stars like the Sun typically survive around ten billion years before their hydrogen fuel begins to run out and they start to die. Over the next ten to hundred thousand years, the stars slowly eject nearly half of their mass in expanding, spherical winds. Then – in a poorly understood phase lasting just 100 to 1,000 years – the stars evolve into a stunning array of geometrically shaped glowing clouds called planetary nebulae.

Just how these extraordinary “star-clouds” are shaped has remained unclear, though Sahai, in several previous papers, put forth a new hypothesis. Based on results from a recent Hubble Space Telescope imaging survey of young planetary nebulae, he proposed that two-sided, or bipolar, high-speed jet-like outflows are the primary means of shaping these objects. The latest study will allow Sahai and his colleagues to test this hypothesis with direct data for the first time.

“Now, in the case of V Hydrae, we can observe the evolution of the jet outflow in real-time,” said Sahai, who together with his colleagues will study the star with the Hubble Space Telescope for three more years.

The new findings also suggest what may be driving the jet outflows. Past models of dying stars predict that accretion discs – swirling rings of matter encircling stars – may trigger jet outflows. The V Hydrae data support the presence of an accretion disc surrounding, not V Hydrae itself, but a companion object around the star. This companion is likely to be another star or even a giant planet too dim to be detected. The authors have also found evidence for an outlying large dense disc in V Hydrae, which could enable the formation of the accretion disc around the companion.

Further support in favor of a companion-driven jet outflow comes from the scientists’ observation that the jet fires in bursts: because the companion orbits the star in a periodic fashion, the accretion disc around it is expected to produce regular spurts of material rather than a steady stream.

The Space Telescope Imaging Spectrograph is managed by NASA’s Goddard Space Flight Center in Greenbelt, Maryland. The Hubble Space Telescope is a project of international cooperation between NASA and the European Space Agency. The California Institute of Technology, Pasadena manages JPL for NASA.

Original Source: NASA/JPL News Release

Image credit: Hubble

Astronomers have known for nearly a century that galaxies are distinct islands of stars, floating apart from each other in space. But it turns out that galaxies are more connected than previously believed because of large-scale “galactic winds” which blow off of galaxies and interact with each other. Researchers from the University of Maryland studied galactic winds in both visible and X-ray light around 10 galaxies, and found that they can often fill an area larger than the galaxy itself. This wind is thought to come from stars and actively feeding black holes.

It was the 17th Century English preacher and poet John Donne who wrote the immortal lines “No man is an island, entire of itself; every man is a piece of the continent, a part of the main.”

Today, astronomers have determined we also do not live in an “island Universe” – that is, a Universe in which the vast agglomerations of gas and stars known as galaxies are wholly independent of the influence of neighboring galaxies and their surrounding environment. Sylvain Veilleux, an astronomer at the University of Maryland, and his colleagues have found important new evidence to support the connectedness of galaxies in the form of unexpectedly large-scale “galactic winds” blowing off of galaxies, altering their surroundings out to distances much farther than previously thought. Galactic winds are the streams of charged particles that blow off of galaxies.

“We are seeing that these galactic winds are blowing off of galaxies on a very large scale,” said Veilleux. “We have detected these winds in both visible light and X-ray light on scales that are sometimes much larger than the galaxies themselves.” The findings are published in the November 2003 issue of the Astronomical Journal, Vol. 126 No. 5 (http://www.journals.uchicago.edu/AJ/journal/issues/v126n5/203224/203224.html). Veilleux’s colleagues in this study were David S. Rupke, a graduate student in physics at the University of Maryland, Patrick L. Shopbell of the California Institute of Technology, Jonathan Bland-Hawthorn of the Anglo-Australian Observatory in Australia, and Gerald N. Cecil of the University of North Carolina at Chapel Hill.

Based on data from the Chandra X-ray Observatory, the Anglo-Australian Observatory located near Coonabarabran in Australia, and the William Herschel Telescope on La Palma in the Canary Islands, Veilleux said these findings have important consequences for the evolution of galaxies and their environment. Veilleux and his colleagues examined the galactic winds surrounding 10 galaxies. Located between 20 and 900 million light years from Earth, the galaxies are in different galaxy clusters and none are in our Milky Way Galaxy’s Local Group cluster. But Veilleux, who is presently on sabbatical at the California Institute of Technology, believes the findings hold for the Milky Way’s galactic wind as well. Galactic winds result from two sources: stars and actively feeding (accreting) giant black holes lurking at the centers of most galaxies. In the first case, Veilleux said, the winds are primarily produced by a combination of the stellar winds blowing off massive stars during their youth and by the titanic explosions known as supernovae that mark their death. Winds produced by these stars are referred to as “starburst-driven.” Starbursts are periods during which large numbers of massive stars are created. These, periods of star creation, in turn, produce strong stellar winds. These massive stars eventually die as supernova. In the second case, he said, enormous (supermassive) and active black holes lurking in the hearts of their host galaxies generate galactic winds. “An ‘active’ black hole is one that is accreting or pulling in a significant amount of the material that is available to it,” Veilleux said. “Such black holes are called ‘active galactic nuclei’ or AGN and the winds they produce are referred to as AGN-driven.”

The Milky Way’s central black hole is an inactive or dormant black hole simply because there isn’t much material in its vicinity available for it to accrete. Measuring the Galactic Wind Veilleux said astronomers are able to detect galactic winds because of the energy emitted when particles that make up the wind collide with other particles. “We can detect these galactic winds because collisions among the charged particles create electromagnetic energy emissions in the form of X rays, visible light and radio waves,” he explained. “These emissions are not uniform in the regions around the galaxies. Rather, they are clumpy, being most notable in the regions where hot gas in the wind collides with colder material from the galaxies themselves or from the intergalactic medium.” The result is filaments of emissions surrounding galaxies in irregular bubble-shaped regions out to at least 65,000 light years from the galaxy centers. Veilleux and his colleagues compared existing Chandra X-ray data with new ground-based observations obtained with a special tunable filter on the Anglo-Australian telescope, which permitted the detection of optical emission down to unprecedented brightness levels. They found the clumpy filaments correlated quite well. This, they say, indicates that galactic winds are indeed influencing the surrounding inter-galactic environment out to previously unknown distances. A Role in the Evolution Galaxies? “What we found is that these winds have a very large zone of influence and probably a strong impact not only on the host galaxy but also on scales in excess of 65,000 light years, possibly well out into the intergalactic medium,” Veilleux said.

Veilleux said the findings mean any comprehensive understanding of long-term galaxy evolution must take into account the flow of gaseous material out of, and back into, the galaxy.

“Galactic winds move at between about 300 and 3000 kilometers per second and if they don’t have enough speed to escape the gravitational pull of the galaxy entirely, it means the material in them would rain back down on the galactic halo and even the disk,” he said. Veilleux explained that such a return “rain” would contribute to the re-enrichment of the host galaxy itself and in this way the more massive galaxies would be able to keep their heavier metals (the sort forged by massive stars during their lives and deaths in supernovae). “The whole issue of the flow of warm gas back into galaxies is very important to understanding the rate at which new stars form.” As for the implications to the Milky Way, Veilleux said the findings for these far away galaxies suggest our Galaxy has its own galactic wind that is creating large-scale bubbles of material around it. Previous findings for the Milky Way have shown direct evidence for a galactic-scale wind at a variety of wavelengths. It is unclear if the Milky Way’s wind is interacting with the nearby Sagittarius dwarf galaxy, which astronomers have discovered is being assimilated into our galaxy through tidal (gravitational) forces. However, Veilleux’s findings have established that galaxies do indeed interact with their surroundings in important ways. “As a result of findings such as these, we now know the closed box or ‘island Universe’ view is not true,” he said.

Original Source: University of Maryland