Sentences with phrase «type of white dwarf star»

Not exact matches

Astronomy is beginning to detect and classify a life of the stars, red, blue and white, giant, middle - sized and dwarf; each type, in its dimensions, particular radiations and brilliance, being subject to a given evolutionary cycle.

• How might the burned - out stars called white dwarfs be brought to ruin by other stars in so - called Type Ia supernovae, inciting the fiery alchemy that yielded much of the iron in our blood and the potassium in our brains?

Researchers have discovered a white dwarf star with an atmosphere dominated by oxygen, a type of white dwarf that has been theorized to exist but not identified to date.

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.

Editor's note: This story was updated January 19, 2018, to clarify the types of stars that become white dwarfs.

Named PH1, the planet goes around two of the four stars, shown close - up here: One is a yellow - white F - type star that is slightly warmer and more luminous than our sun; the other, at the 11 o'clock position, is a red dwarf, cooler and dimmer than the sun.

All type 1a evolve from a type of star called a white dwarf, but pinning down exactly which white dwarfs are supernova precursors could lead to much more precise measurements of dark energy — and even reveal its true nature.

Another, less common kind of supernova, type 1a, occurs when a remnant of a star called a white dwarf steals matter from a companion star until the white dwarf explodes (SN: 4/30/16, p. 20).

At first glance this exploding star had all the features of a type Ia supernova, which happens when a small, dense white dwarf star steals material from an orbiting companion and then explodes.

A type Ia supernova represents the total destruction of a white dwarf star by one of two possible scenarios.

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.

Astronomers have identified a white dwarf star in our galaxy that may be the leftover remains of a recently discovered type of supernova.

Type Iax supernovae may be caused by the partial destruction of a white dwarf star in such an explosion.

Type Ia supernovae are caused by the complete destruction of a white dwarf star in a thermonuclear explosion.

[3] Type Ia Supernovae occur when an accreting white dwarf in a binary star system slowly gains mass from its companion until it reaches a limit that triggers the nuclear fusion of carbon.

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.

Astronomers thought white dwarfs gained mass from a companion star, but about half of the type Ia supernovae show no signs of a companion.

Vega is a slightly bluish, white main sequence dwarf star of spectral and luminosity type A0 V, like Sirius.

In Type 1 supernovas, one star in the binary system is a white dwarf, a dying star that has consumed almost all of its hydrogen.

A Type Ia supernova results from a white dwarf that's part of a binary system (that is, one that shares an orbit with another star) and was about twice the size of our sun during its life.

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).

Gamma Pavonis is a yellowish - white main sequence dwarf star of spectral and luminosity type F6 - 8 V.

The stars observed cover almost the entire range of star - types — main sequence, red giants, and white dwarfs.

Star A is a white dwarf stellar remnant of spectral and luminosity type DA2 / VII.

Unlike Sol, it is a slightly bluish, white main sequence dwarf star of spectral and luminosity type A0 - 1 Vm.

Type Ia supernovae are fairly rare in the nearby Universe and represent the explosion of at least one white dwarf star in a binary system.

While it's known that Type 1a supernovae form from collapsing white dwarfs — the densest forms of matter after black holes and neutron stars — their formation theories come in two flavors: the single degenerate scenario in which a normal star is consumed by a white dwarf; and the double degenerate scenario in which two white dwarfs merge.

This star is a white - yellow main sequence dwarf star of spectral and luminosity type F6 V, with almost 1.3 times Sol's mass (NASA Star and Exoplanet Database; and David F. Gray, 1992), 1.2 5o 1.3 times its diameter (von Belle and von Braun, 2009, HD 30652 in Table 4, page 7; Perrin and Karoji, 1987; NASA Star and Exoplanet Database; and Kenneth R. Lang, 1980), and over 2.6 times of its bolometric luminosity (NASA Star and Exoplanet Database; and Kenneth R. Lang, 19star is a white - yellow main sequence dwarf star of spectral and luminosity type F6 V, with almost 1.3 times Sol's mass (NASA Star and Exoplanet Database; and David F. Gray, 1992), 1.2 5o 1.3 times its diameter (von Belle and von Braun, 2009, HD 30652 in Table 4, page 7; Perrin and Karoji, 1987; NASA Star and Exoplanet Database; and Kenneth R. Lang, 1980), and over 2.6 times of its bolometric luminosity (NASA Star and Exoplanet Database; and Kenneth R. Lang, 19star of spectral and luminosity type F6 V, with almost 1.3 times Sol's mass (NASA Star and Exoplanet Database; and David F. Gray, 1992), 1.2 5o 1.3 times its diameter (von Belle and von Braun, 2009, HD 30652 in Table 4, page 7; Perrin and Karoji, 1987; NASA Star and Exoplanet Database; and Kenneth R. Lang, 1980), and over 2.6 times of its bolometric luminosity (NASA Star and Exoplanet Database; and Kenneth R. Lang, 19Star and Exoplanet Database; and David F. Gray, 1992), 1.2 5o 1.3 times its diameter (von Belle and von Braun, 2009, HD 30652 in Table 4, page 7; Perrin and Karoji, 1987; NASA Star and Exoplanet Database; and Kenneth R. Lang, 1980), and over 2.6 times of its bolometric luminosity (NASA Star and Exoplanet Database; and Kenneth R. Lang, 19Star and Exoplanet Database; and Kenneth R. Lang, 1980), and over 2.6 times of its bolometric luminosity (NASA Star and Exoplanet Database; and Kenneth R. Lang, 19Star and Exoplanet Database; and Kenneth R. Lang, 1980).

Star A is bluish white main sequence dwarf of spectral and luminosity type A3 Va (NASA Stars and Exoplanet Database; Gray et al, 2003; and Garrison and Beattie, 1998).

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

In 2003, astronomers announced that they had discovered that iron from supernovae of the first stars (possibly from Type Ia supernovae involving white dwarfs) indicate that «massive chemically enriched galaxies formed» within one billion years after the Big Bang, and so the first stars may have preceded the birth of supermassive black holes (more from Astronomy Picture of the Day, ESA, and Freudling et al, 2003).

This star is a main - sequence white - yellow dwarf star of spectral and luminosity type F6 - 7 V. Gamma Leporis has about 1.2 times Sol's mass, about 1.3 times its diameter, and about 2.6 times of its luminosity.

Lecture 12 of Dr. Bruce Betts» 2014 online Introductory Planetary Science and Astronomy course covers the Sun (physical characteristics, zones, solar cycle, sunspots, flares, coronal mass ejections, fusion, etc.) and Stars and Stellar Evolution (star types and colors, evolution, HR Diagrams, birth and death phases, white dwarfs, neutron stars, black hoStars and Stellar Evolution (star types and colors, evolution, HR Diagrams, birth and death phases, white dwarfs, neutron stars, black hostars, black holes).

If the white dwarf accretes enough material to reach the Chandrasekhar limit, the maximum mass of a stable white dwarf star (1.4 solar mass), it will likely explode as a Type Ia supernova.