Sentences with phrase «for white dwarf stars»

It was named in honor of Indian - American physicist Subrahmanyan Chandrasekhar who is known for determining the mass limit for white dwarf stars to become neutron stars.

Not exact matches

Creating so much oxygen takes a fiercer nuclear furnace than is needed for a carbon - rich mixture, so the stars that became these white dwarfs must have been hot and massive.

For the first time, scientists using NASA's Hubble Space Telescope have witnessed a massive object with the makeup of a comet being ripped apart and scattered in the atmosphere of a white dwarf, the burned - out remains of a compact star.

The unseen movers are fast - moving white dwarf stars that could account for as much as one - third of the galaxy's dark matter.

The diffuse cloud in this image, taken with the Carnegie Institution for Science's Swope telescope in Chile, is the shell of hot hydrogen gas ejected by a white dwarf star on March 11, 1437.

The event was what's known as a classical nova explosion, which occurs when a dense stellar corpse called a white dwarf steals enough material from an ordinary companion star for its gas to spontaneously ignite.

For the past two years, Winget and his colleagues at the University of Texas at Austin and Sandia National Laboratory in Albuquerque, New Mexico, have been creating searing plasmas that are, in effect, miniature versions of white dwarfs, ancient stars that have burned up all their nuclear fuel.

WHAT LIES WITHIN The inner structure of a white dwarf star (shown in this artist's impression) has been mapped for the first time — and it's more oxygen - rich than expected.

Cruelly, the dense white dwarf star could also be headed for a violent demise unlike anything we've ever seen.

In 2014, scientists found another reason to rejoice in your genes» deterioration: White dwarf stars, like the remnant that will remain at the end of the sun's life, eat rocky planets like Earth for their last meal.

NEWSPAPER obituaries of Subrahmanyan Chandrasekhar, who died last month aged 84, all highlighted the single achievement for which he will be best remembered — his work on white dwarf stars.

Professor Mould and his PhD student Syed Uddin at the Swinburne Centre for Astrophysics and Supercomputing and the ARC Centre of Excellence for All - sky Astrophysics (CAASTRO) assumed that these supernova explosions happen when a white dwarf reaches a critical mass or after colliding with other stars to «tip it over the edge».

Neither study searched for the stars responsible for so - called type Ia supernovae, which are explosions of white dwarf stars that have grown overweight by feasting on material from a companion star.

Observations of the explosions of white dwarf stars in binary systems, so - called Type Ia supernovae, in the 1990s then led scientists to the conclusion that a third component, dark energy, made up 68 % of the cosmos, and is responsible for driving an acceleration in the expansion of the universe.

And even then, the planet would have to orbit a special kind of star, a white dwarf, for the CFCs to show up.

This is too small for normal stars or white dwarfs, but fine for neutron stars.

Those remnants went into orbit around the white dwarf — much like the rings around Saturn, Zuckerman said — before eventually spiraling onto the star itself, bringing with them the building blocks for life.

As Vega is so much bigger and hotter than Sol, however, the star will exhaust its core hydrogen after only another 650 million years or so (for a total life of around a billion years) and turn into a red giant or Cepheid variable before puffing away its outer layers to reveal a remnant core as a white dwarf.

Zeta Doradus is a main sequence dwarf star of spectral and luminosity type F7 V but has been classed as white as F6 and as yellow as F9 (Lagrange et al, 2009, page 14 for HD 33262; Trilling et al, 2008, page 26; NASA Stars and Exoplanet Database; and SIMBAD).

Even for these more massive stars, however, if the residual mass in the core is less than 1.4 solar masses (the Chandrasekhar limit), the stellar remnant will become a white dwarf.

Scientists from a large international collaboration (Oxford, AWE, CEA, LULI, Observatoire de Paris, University of Michigan and University of York) have succeeded for the first time to generate a laboratory analogue of a strong shock that takes place when matter falls at very high speed on the surface of extremely dense stars called white dwarfs.

Researchers using NASA's Hubble Space Telescope have observed, for the first time ever, an enormous object with the composition of a comet being shredded and scattered by a white dwarf, the burned - out husk of a massive star.

Its mass and diameter are consistent with the theoretical size for a carbon - core white dwarf, one that may have evolved from a 5.05 +0.374 / -0.276 Solar - mass, B - type main - sequence star about 124 + / - 5 million years ago, after 101 to 126 million years as a giant star (Liebert et al, 2005; and Ken Croswell, 2005).

Peering deep into the Milky Way's crowded central hub of stars, Hubble researchers have uncovered for the first time a population of ancient white dwarfs — smoldering remnants of once - vibrant stars that inhabited the core.

David Aguilar, Harvard - Smithsonian Center for Astrophysics — larger «day» and «night» images At maximum brightness, Mira would light up a hypothetical planetary companion, but at its most dark, the giant star's small, hot white dwarf companion would become visible (more discussion with illustration).

UC Santa Barbara Astrophysicists are the first to identify two white dwarf stars in an eclipsing binary system, allowing for the first direct radius measurement of a rare white dwarf.

From the original description, the team knew they were looking for a nova eruption — an extremely powerful explosion, where a white dwarf is fed by hydrogen from a nearby star.

A different set of spectral peculiarity symbols are used for white dwarfs than for other types of stars:

Building on past observations of the white dwarf called SDSSJ1043 +0855 (the dead core of a star that originally was a few times the mass of the Sun), which has been known to be gobbling up rocky material in its orbit for almost a decade, the team used Keck Observatory's HIRES instrument fitted to the 10 - meter Keck I telescope as well as data from the Hubble Space Telescope to measure and characterize the material being accreted by the star.

Our choice of calcium - carbonate as a potential carrier of the carbon provides a natural way for it to be locked up in the planet and eventually delivered to the white dwarf star, is entirely consistent with the observations in hand, and of course is suggestive.

Luminosity class 0 or Ia + is used for hypergiants, class I for supergiants, class II for bright giants, class III for regular giants, class IV for sub-giants, class V for main - sequence stars, class sd (or VI) for sub-dwarfs, and class D (or VII) for white dwarfs.

Nominal luminosity class VII (and sometimes higher numerals) is now rarely used for white dwarf or «hot sub-dwarf» classes, since the temperature - letters of the main sequence and giant stars no longer apply to white dwarfs.

The class D (for Degenerate) is the modern classification used for white dwarfs — low - mass stars that are no longer undergoing nuclear fusion and have shrunk to planetary size, slowly cooling down.

The sequence has been expanded with classes for other stars and star - like objects that do not fit in the classical system, such as class D for white dwarfs and classes S and C for carbon stars.

Using NASA's Hubble Space Telescope, astronomers have captured for the first time snapshots of fledgling white dwarf stars beginning their slow - paced, 40 - million - year migration from the crowded centre of giant globular cluster 47 Tucanae to the less populated suburbs.

The story began with observations by Justin Steinfadt, a UCSB physics graduate student who has been monitoring white dwarf stars as part of his Ph.D. thesis with Lars Bildsten, a professor and permanent member of UCSB's Kavli Institute for Theoretical Physics, and Steve Howell, an astronomer at the National Optical Astronomy Observatory (NOAO) in Tucson, Ariz..

Astrophysicists at UC Santa Barbara are the first scientists to identify two white dwarf stars in an eclipsing binary system, allowing for the first direct radius measurement of a rare white dwarf composed of pure helium.