Sentences with phrase «white dwarf star as»

In their new study, the Leicester - led team assesses whether these laws are the same within the hot, dense conditions in the atmosphere of a dying white dwarf star as here on Earth.

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..

Not exact matches

So, too, do astrophysical exotica such as neutron stars and white dwarfs — the remnants left by normal stars when they die.

The researchers found that relatively cool accretion discs around young stars, whose inner edges can be several times the size of the Sun, show the same behaviour as the hot, violent accretion discs around planet - sized white dwarfs, city - sized black holes and supermassive black holes as large as the entire Solar system, supporting the universality of accretion physics.

The study, «Accretion - induced variability links young stellar objects, white dwarfs, and black holes», which is published in the journal Science Advances, shows how the «flickering» in the visible brightness of young stellar objects (YSOs)-- very young stars in the final stages of formation — is similar to the flickering seen from black holes or white dwarfs as they violently pull matter from their surroundings in a process known as accretion.

Brown dwarfs, less massive than stars, are nearly dark, as are collapsed stars — white dwarfs, neutron stars, and black holes.

As relatively small stars (those less than ten times the mass of our sun) near the end of their lives, they throw off their outer layers and become white dwarf stars, which are very dense.

These icy bodies apparently survived the star's evolution as it became a bloated red giant and then collapsed to a small, dense white dwarf.

In this artist's conception, a Ceres - like asteroid is slowly disintegrating as it orbits a white dwarf star.

Astronomers think white dwarfs must not be stars so much as the corpses of stars.

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

CANNIBAL ZOMBIE STAR Dead stars called white dwarfs (left) steal material from ordinary companion stars (right), as shown in this artist's illustration.

We once thought that dark matter might be made up of large objects such as black holes or exotic types of faint stars — neutron stars or white dwarfs — that are nearly invisible to our telescopes.

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.

Imagine being able to view microscopic aspects of a classical nova, a massive stellar explosion on the surface of a white dwarf star (about as big as Earth), in a laboratory rather than from afar via a telescope.

That happens if it has a companion star, as most stars in the galaxy do, and the white dwarf orbits it closely enough to steal material from it.

But von Hippel, Gilmore and their colleagues used the Hubble Space Telescope, and this allowed them to identify and measure the temperature of white dwarfs as faint as 25th magnitude, which is about 100 million times fainter than any star visible with the naked eye.

Known as 2014J, this was a Type la supernova caused by the explosion of a white dwarf star, the inner core of star once it has run out of nuclear fuel and ejected its outer layers.

But some scientists have suggested the fast - moving stars near the cluster centres could instead result from the gravity of many dim, dead stars such as white dwarfs or neutron stars.

When Sigurdsson and colleagues analyzed images of the white dwarf from the Hubble Space Telescope, they concluded that the distant, unseen companion is not a low - mass star, as many researchers had thought, but a planet with about 2.5 times the mass of Jupiter.

The first hint of the kamikaze asteroids came about 40 years ago, when astronomers discovered heavy elements such as magnesium in the spectra of some white dwarf stars.

The discovery came as a complete surprise, as the team assumed the dusty white dwarf was a single star but co-author Dr Steven Parsons (University of Valparaíso and University of Sheffield), an expert in double star (or binary) systems noticed the tell - tale signs.

EUVE will seek out white dwarfs that are coupled with normal stars as binary pairs.

The explosion was a Type Ia supernova, the most luminous variety, which occurred when a small, dense star known as a white dwarf blew up about 7000 light - years from Earth.

PSR J1713 +0747, as it is known, has a tiny white dwarf companion star, and the two orbit each other exceptionally predictably.

(Part of an ordinary star or white dwarf also exists as this energy, but a much smaller fraction.)

The spectra of the white dwarfs indicate the stars are 53 % as massive as the sun.

As general relativity predicts, light from the background star bent around the white dwarf, distorted by its gravitational field.

The white dwarf accretes material from the companion star, then at some point, it might explode as a type Ia supernova.

Specifically, the most energetic iron emission they studied is characteristic of so - called x-ray binary starsduos comprised of a dense stellar object such as a white dwarf star, a neutron star or a black hole that collects matter from a less dense companion, emitting x-rays in the process.

Kailash Sahu and colleagues at the Space Telescope Science Institute in Baltimore, Maryland, measured bending light from white dwarf Stein 2051 B as it moved in front of another star over two years.

The Garden Sprinkler (center) is an aging star, not yet a white dwarf, that is shedding its atmosphere in pulsing jets, like the arcs of water that hang in the air as a lawn sprinkler twirls.

What remains behind is a nearly naked core of carbon and oxygen, which collapses to form a white dwarf star, roughly the size of Earth but 100,000 times as dense.

White - dwarf stars (circled) cool as they become older.

Today the central star is of mag 16.6 and a high temperature of some 60,000 K, which will probably cool down as a white dwarf over the coming tens of billions of years.

The burned - out star, called a white dwarf, appears as a white dot in the center.

Today, a UCLA - led team of scientists reports that it has discovered the existence of a white dwarf star whose atmosphere is rich in carbon and nitrogen, as well as in oxygen and hydrogen, the components of water.

Type Ia supernovas are known to form when a white dwarf merges with another star, like a puffed - up red giant (as opposed to Type II supernovas, which form when a single star dies and collapses on itself).

The sun will eventually lose most of its mass as it becomes a white dwarf, and could come to resemble other burnt - out star systems spotted by NASA's Spitzer Space Telescope in a 2009 study.

In most instances, especially among low - mass stars, the distended outer envelope of the star simply drifts off into space, while the core settles down as a white dwarf.

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 dwarAs 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 dwaras 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).

As stars like our sun age, they puff up into red giants and then gradually lose about half or more of their mass, shrinking into skeletons of stars, called white dwarfs.

12 systems were resolved as new binaries, including the discovery of a new white dwarf companion to the star HD8049.

White dwarfs form as the outer layers of a low - mass red giant star puff out to make a planetary nebula.

It may be only about 225 to 250 million years old (Liebert et al, 2005; and Ken Croswell, 2005), but being so much bigger and hotter than Sol, the star will exhaust its core hydrogen within only 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.

«You can see bulges in distant galaxies, but you can not resolve the very faint stars, such as the white dwarfs.

The remnant of the star that is left is an intensely hot white dwarf with a surface temperature as high as 100 000K.

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).

Nicknamed «the Pup» as the much smaller companion to the Dog Star, this much dimmer object is a white dwarf (DA2 - 5 or A2 - 5 VII).