PSR J1713 +0747, as it is known, has a tiny white
dwarf companion star, and the two orbit each other exceptionally predictably.
The Sun, the 12 brightest stars of the Northern Hemisphere and the white
dwarf companion stars to Sirius and Procyon are shown.
Not exact matches
The extremely strong gravity of a massive neutron
star in orbit with a
companion white
dwarf star puts competing theories of gravity to a test more stringent than any available before
Matter falling from a
companion star onto a white
dwarf might have induced a thermonuclear chain reaction that forced the
dwarf to expand radically without exploding into a more common nova, Bond notes.
Close encounter Tracing the trajectory of the
star and its brown
dwarf companion back in time, Mamajek's team found with 98 % confidence that Scholz's
star passed within the Solar System's Oort cloud, a reservoir of comets, about 70,000 years ago.
CANNIBAL ZOMBIE STAR Dead
stars called white
dwarfs (left) steal material from ordinary
companion stars (right), as shown in this artist's illustration.
The
companion star may have dumped its gas on the white
dwarf until the added weight sparked a thermonuclear detonation.
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.
In all, the team found 17 candidate brown
dwarf companions to red
dwarf stars, one brown
dwarf pair, and one brown
dwarf with a planetary
companion.
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.
A nova can occur if the strong gravity of a white
dwarf pulls material from its orbiting
companion star.
The measurement is the distance to SS Cygni, a
star system consisting of a white
dwarf plus a
companion.
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.
Sandage's preferred method is to use type Ia supernovae, which arise when a white
dwarf star gathers material from a
companion and explodes.
These so - called supersoft sources are now thought to be white
dwarf stars that cannibalize their stellar
companions and then, in many cases, explode
«Right now, the
star and the brown
dwarf are locked in a honeymoon phase, where they both turn the same face to each other all the time,» says Beatty, «but in the future, the
star will swell up and engulf its
companion completely.»
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.
However, in a
star - brown
dwarf binary, the
star's rotation is much slower than the brown
dwarf's orbital motion, so the
companion is dragged inward.
[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.
«Our knowledge of binary evolution suggests that, if the
companion star can survive the transition, brown
dwarfs should be common in this type of system.
In the background is the
star's binary
companion, Kepler - 13B, and the third member of the multiple -
star system is the orange
dwarf star Kepler - 13C.
Such a supernova is supposed to result when a larger
companion star dumps material onto the white
dwarf, triggering a runaway nuclear reaction that annihilates the small
star.
Astronomers have detected a sub-stellar object that used to be a
star, after being consumed by its white
dwarf companion.
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.
Such a shock could not have been produced if the
companion were another white
dwarf star.
The UCSB - led research implies that the white
dwarf was stealing matter from a much larger
companion star — approximately 20 times the radius of the sun — which caused the white
dwarf to explode.
Astronomers thought white
dwarfs gained mass from a
companion star, but about half of the type Ia supernovae show no signs of a
companion.
The first so - called helium nova, the possible result of a large white
dwarf sucking material from a hydrogen - deficient
companion star, may be a precursor to a supernova
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.
Not only do
stars provide a ready energy source of radiated light and heat, but the mass and gravitational pull of
stars flat - out
dwarfs the summed masses and pulls of any orbiting
companions.
The traditional view held that a white
dwarf, locked in a binary pairing with another
star, sucked matter from its
companion, growing ever larger in size until it could no longer support its own weight.
In this theory material from the
companion star is accreted onto the white
dwarf until its mass reaches a limit, leading to a dramatic explosion.
The
star also has a small
companion, a red
dwarf star that lies about 1000 times as far away as Earth's distance from the sun.
Both occur in systems where two
stars orbit each other: a white
dwarf sucks away the outer layers of a larger
companion star until the smaller
star reaches a critical mass, causing an explosion.
The second theory proposes that only one
star in the system is a white
dwarf, while its
companion is a normal
star.
This red
dwarf pulls on the 55 Cancri system, and because all five planets in the system — and their host
star — are such a tight - knit family, they behave like ice skaters holding hands, so that the
companion star's tugs cause them all to do somersaults in space.
Or it may be influenced by a tidal tug from the
star's red
dwarf binary
companion (HR 4796B), located at least 54 billion miles from the primary
star.
Between August 24 and September 18, 2006, two teams of astronomers announced the discovery and direct imaging of a spectral type - T, methane brown
dwarf companion (T7.5 + / - 0.5) to this
star (PSU press release; Luhman et al, 2006; and Mugrauer et al 2006).
© Estate of John Whatmough — larger image (Artwork from Extrasolar Visions, used with permission from Whatmough) Glowing red through gravitational contraction, the candidate brown
dwarf companion to Proxima Centauri is depicted with two moons (one eclipsing the flare
star) with distant Alpha Centauri A and B at upper right, as imagined by Whatmough.
This much dimmer
companion star is a main sequence, orange - red
dwarf (K0 - 1 V).
In 2006, astronomers discovered a very dim («mid-range»), red
dwarf companion to HD 189733 A of spectral and luminosity type M V. Observed at a separation of 216 AUs from
Star A, the companion star has a clockwise orbit that is nearly perpendicular to the orbital plane of transiting planet b around Star A (HD 189733 b or
Star A, the
companion star has a clockwise orbit that is nearly perpendicular to the orbital plane of transiting planet b around Star A (HD 189733 b or
star has a clockwise orbit that is nearly perpendicular to the orbital plane of transiting planet b around
Star A (HD 189733 b or
Star A (HD 189733 b or Ab).
The closest
star to the sun, proxima centauri, a
companion of alpha centauri, is also a red
dwarf.
Discovered to be a faint
companion of
Stars Aab by Ragnar Furuhjelm, Capella C is a red
dwarf star of spectral and luminosity type M1 V.
Discoveries of Sun - like
stars with host exoplanets as well as red
dwarf companions have been common, and many appear to be old and stable enough for life to have evolved (RAS new releases of April 16 and April 19, 2011; and University of St. Andrews press release).
Its red
dwarf companion B was first detected through astrometric perturbations of
Star A's motion in 1976 by Sarah Lee Lippincott and J.J. Lanning.
Between August 24 and September 18, 2006, two teams of astronomers announced the discovery and direct imaging of a brown
dwarf companion to this
star (press release; Luhman et al, 2006; and Mugrauer et al 2006 — more below).
NGC 3359 appears to be devouring a much smaller gas rich
dwarf galaxy, nicknamed the Little Cub, which contains 10,000 times fewer
stars than its larger
companion.
A binary
star system (consisting of a white
dwarf and a
companion star) that rapidly brightens, then slowly fades back to normal.