Sentences with phrase «binary pair»

NASA (Krist, et al, 1999) Until the discovery of superflares by stars like Kappa Ceti, enormous coronal mass ejections releasing energy from 100 to 10 million times greater than a typical Solar flare by stars of spectral classes F8 to G8 were thought to be limited to very young stars — like this magnetically - driven outburst by the million - year - old binary pair of pre-main-sequence stars, XZ Tauri AB.

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

Note: Special thanks to Andrew Tribick about the 2012 discovery of a T8.5 brown dwarf and to David Bellomy for pointing out the implausibility of the reported semi-major axis for the inner binary pair Aab and encouraging us to derive a more plausible, average orbital separation.

In 1996, two teams of astronomers announced the possible detection of a planetary transit eclipse of the close binary pair CM Draconis Aab (Guinan et al, 1998; Martin and Deeg, 1996; and Guinan et al, 1996).

NASA (Krist, et al, 1999) Until the discovery of superflares by stars like Groombridge 1830, enormous coronal mass ejections releasing energy from 100 to 10 million times greater than a typical Solar flare by stars of spectral classes F8 to G8 were thought to be limited to very young stars — like this magnetically - driven outburst by the million - year - old binary pair of pre-main-sequence stars, XZ Tauri AB.

From the perspective of an observer on Earth, the orbit of Star A and the BC tight binary pair exhibit a very elongated and narrow ellipse whose separation has varied from 4.7» in 1880 to less than 0.4» in 1969 (Kaj Aage Gunnar Strand, 1937; A. Gennaro, 1940; L. Bennendijk, 1955; Worley and Heintz, 1983; and Wulff Dieter Heintz, 1963 to 1997; among others).

In 1996, two teams of astronomers announced the possible detection of a planetary transit eclipse of the close binary pair CM Draconis Aab, which has yet to be confirmed (further details below).

Its sky would contain two suns, and the more distant binary pair would appear as two very bright stars, visible even during daylight.

The new study may help researchers calculate how often these black holes will form binary pairs and then merge, Loeb says.

If each galaxy possesses a central supermassive black hole, they will form a bound binary pair at the center of the merged galaxy before ultimately coalescing themselves.

The star is located roughly a fifth of a light - year from the AB binary pair and, if gravitationally bound to it, may have an orbital period of around half a million years.

According to the Astronomisches Rechen - Institut's Catalogue of Nearby Stars (ARICNS) notes on Star B, the BC companion binary pair has an observed separation of about 286 AUs (34.0» at a HIPPARCOS parallax of 0.11905 + / -0.00062») from primary pair Aab at an orbital inclination of 247 ° (1955) from the perspective of an observer on Earth.

The galaxy mergers that bring two supermassive black holes close together are considered to be a common process in the universe, so astronomers expect that such binary pairs should be common.

According to the Yale Bright Star Catalogue's notes entry for HR 5618, a variation in the light curve for this close spectroscopic binary pair appears to be caused by mass transfer, which is supported by observations of gaseous streams between the stars.

reduces the likelihood of stable planetary orbits at increasing distances from each star or binary pair Alan Hale, 1994.

However, in the case of HD 98800B, the dust particles do not evenly fill out the inner disk as expected, due to either planets or the diskless binary pair sitting 50 AU away and gravitationally influencing the movement of dust particles.

Its well known and attractive, visual binary pair of a bright yellow star and a reddish - violet to pink companion was discovered in 1780 by Sir William Herschel (1738 - 1822), who was born Friedrich Wilhelm Herschel and subsequently discovered the planet Uranus in 1781 — which led to his appointment in 1782 as private astronomer to the King of England.

Different wavelengths and images of the 0.032 arcseconds (or 32 mas) Theta 1 Ori C binary Pair.

On the other hand, the wide binary pairs Aab and Bab are separated by an «average» distance of about 21.2 AUs (of a semi-major axis of 2.533» at 27.3 ly) in an elliptical orbit (e = 0.412) of 59.9 years, so that the two star pairs get as close as 12.5 AUs and as far away as 39.9 AUs (Wulff Dieter Heintz, 1996; revising earlier earlier estimates, including Mason et al, 1995).

NASA (Krist, et al, 1999) Instabilities in the strong magnetic fields of young stars lead to massive stellar flares (coronal mass ejections)-- like this magnetically - driven outburst by the million - year - old binary pair of pre-main-sequence stars, XZ Tauri AB.

The planet, named Kepler 16 b for the NASA Kepler spacecraft that spotted it, revolves around two stars locked in a tight binary pairing; the planet's wide, nearly circular orbit keeps it well outside the stars» orbital dance.

In turn, this close binary pair (Aab) has another companion binary of stars (BC).

The stars being studied were identified as members of a binary pair because they periodically move closer to and further from Earth — the hallmark of an orbiting pair of stars.

The system is arranged as two binary pairs that orbit each other at a distance more than a thousand times that between the Earth and our sun.

Lower velocity runaway stars can be produced when one half of a binary pair explodes as a supernova, blasting its partner away.

Bond's team doesn't yet know what triggered the strange flare, although spectra suggest that the star is a binary pair.

But this is the first time a binary pair has been found to host a multi-planet system.

The situation, says former LHCb spokesperson and University of Oxford physicist Guy Wilkinson, is roughly analogous to a planetary system in which the light quark is akin to a planet orbiting a binary pair of massive stars.

Two teams, led by Saul Perlmutter of the Lawrence Berkeley Laboratory in California and Alex Filippenko of the University of California at Berkeley, observed scores of distant «Type Ia» supernovae, in which one star in a binary pair explodes.

Lead author of the study, Mr M. Mirac Serim, a senior PhD student working under the supervision of Prof Altan Baykal, said, «This pulsar is particularly interesting, since as well as orbiting its partner star as part of a binary pair, it is also still surrounded by the remnants of the supernova explosion which created it.»

NASA will submit a formal name (or names) to the International Astronomical Union after the flyby, based on whether MU69 turns out to be a single body, binary pair or other system.

This artist's rendition depicts the probe's target as a binary pair.

Current candidates range from Mjölnir (the hammer of the Norse god Thor) to Z'ha» dum (a planet from Babylon 5) to Peanut, Almond and Cashew — multiple name options may be necessary if the object is a binary pair.

Many believe the system's larger, brighter and more sunlike stars, the binary pair Alpha Centauri A and B, offer better prospects for life - friendly worlds, even though all previous planet hunts there have come up empty - handed.

After the flyby, NASA will submit a formal name to the International Astronomical Union based on whether Ultima Thule is a single object, a binary pair or a multi-object system.

The new study identifies eight star systems where the orbital axis for a binary pair lines up with the long axis of symmetry for the nebula — suggesting that theorists were right all along.

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.

The favored alternative at present is the so - called double - degenerate scenario, in which two white dwarfs locked in a binary pairing spiral inward and merge, triggering an explosion.

According to the Astronomisches Rechen - Institut's Catalogue of Nearby Stars (ARICNS), Heintz's 1994 analysis of Mu Herculis Aa also derived an updated period of 65 years which would imply a semi-major axis of just under 17.2 AUs, assuming that the combined mass of Mu Herculis Aab is 1.2 times that of Sol's (which is consistent with Wanner's 1967 estimate of the mass ratio of 0.50 (+ / - 0.04) for the binary pair BC — combined — to the primary).

NASA — larger image Mu Herculis BC are dim red dwarf stars, like the binary pair Gliese 623 A (M2.5 V) and B (M5.8 Ve)-- at lower right.

Astronomers studying data from the National Science Foundation's Very Long Baseline Array and other telescopes have concluded that a binary pair of stars forming an energetic microquasar was blasted out of the cluster in which it was born by a supernova.

The stars in the binary pairs orbit around each other, and the two pairs also circle each other like choreographed ballerinas.

reduces the likelihood of stable planetary orbits at increasing distances from each star or binary pair (Alan Hale, 1994).

Although the four stars are gravitationally bound, the distance separating the two binary pairs is about 50 astronomical units (AU)-- slightly more than the average distance between our sun and Pluto.

Given that the closest separation of the stars in the binary pair Aab is around 0.8 AU (given an ecccentricity of 0.53), however, such a planetary orbit appears unlikely to be stable.

A recent analysis of radial velocities, however, discusses the possibility of a Bb companion as a orange - red (late K - type) dwarf star based on suspected mass ratios among the binary pairs without any mention of the 1996 brown dwarf finding (Griffin, 1998, pp. 293 - 294).

Both would have been born from massive stars that evolved in close proximity in ancient star factories as a binary pair, eventually dying as supernovas.