scholarly journals The Formation of Population III Binaries from Cosmological Initial Conditions

Science ◽  
2009 ◽  
Vol 325 (5940) ◽  
pp. 601-605 ◽  
Author(s):  
Matthew J. Turk ◽  
Tom Abel ◽  
Brian O'Shea
Keyword(s):  
Molecular Hydrogen ◽  
Initial Conditions ◽  
Binary Star ◽  
The Sun ◽  
Star System ◽  
Mass Ratio ◽  
Gas Reservoir ◽  
First Stars ◽  
Hydrogen Lines ◽  
Binary Star System

Previous high-resolution cosmological simulations predicted that the first stars to appear in the early universe were very massive and formed in isolation. Here, we discuss a cosmological simulation in which the central 50 M⊙ (where M⊙ is the mass of the Sun) clump breaks up into two cores having a mass ratio of two to one, with one fragment collapsing to densities of 10−8 grams per cubic centimeter. The second fragment, at a distance of ~800 astronomical units, is also optically thick to its own cooling radiation from molecular hydrogen lines but is still able to cool via collision-induced emission. The two dense peaks will continue to accrete from the surrounding cold gas reservoir over a period of ~105 years and will likely form a binary star system.

scholarly journals A terrestrial planet in a ~1-AU orbit around one member of a ∼15-AU binary

Science ◽  
2014 ◽  
Vol 345 (6192) ◽  
pp. 46-49 ◽  
Author(s):  
A. Gould ◽  
A. Udalski ◽  
I.-G. Shin ◽  
I. Porritt ◽  
J. Skowron ◽  
...  
Keyword(s):  
Binary Systems ◽  
Planet Formation ◽  
Binary Star ◽  
Terrestrial Planet ◽  
Search Strategies ◽  
The Sun ◽  
Star System ◽  
Low Mass ◽  
Formation And Evolution ◽  
Binary Star System

Using gravitational microlensing, we detected a cold terrestrial planet orbiting one member of a binary star system. The planet has low mass (twice Earth’s) and lies projected at ~0.8 astronomical units (AU) from its host star, about the distance between Earth and the Sun. However, the planet’s temperature is much lower, <60 Kelvin, because the host star is only 0.10 to 0.15 solar masses and therefore more than 400 times less luminous than the Sun. The host itself orbits a slightly more massive companion with projected separation of 10 to 15 AU. This detection is consistent with such systems being very common. Straightforward modification of current microlensing search strategies could increase sensitivity to planets in binary systems. With more detections, such binary-star planetary systems could constrain models of planet formation and evolution.

scholarly journals An Important Binary Star System

Nature ◽  
1942 ◽  
Vol 150 (3810) ◽  
pp. 545-545
Keyword(s):  
Binary Star ◽  
Star System ◽  
Binary Star System

scholarly journals KOI-3278: A Self-Lensing Binary Star System

Science ◽  
2014 ◽  
Vol 344 (6181) ◽  
pp. 275-277 ◽  
Author(s):  
E. Kruse ◽  
E. Agol
Keyword(s):  
Binary Star ◽  
Star System ◽  
Binary Star System

scholarly journals Impact flux of asteroids and water transport to the habitable zone in binary star systems

2014 ◽  
Vol 9 (S310) ◽  
pp. 86-87
Author(s):  
D. Bancelin ◽  
E. Pilat-Lohinger ◽  
S. Eggl ◽  
R. Dvorak
Keyword(s):  
Binary Star ◽  
Stellar System ◽  
Terrestrial Planet ◽  
Solar Neighborhood ◽  
Planetary Motion ◽  
Habitable Zone ◽  
Star System ◽  
Single Star ◽  
Multiple Systems ◽  
Binary Star System

AbstractBy now, observations of exoplanets have found more than 50 binary star systems hosting 71 planets. We expect these numbers to increase as more than 70% of the main sequence stars in the solar neighborhood are members of binary or multiple systems. The planetary motion in such systems depends strongly on both the parameters of the stellar system (stellar separation and eccentricity) and the architecture of the planetary system (number of planets and their orbital behaviour). In case a terrestrial planet moves in the so-called habitable zone (HZ) of its host star, the habitability of this planet depends on many parameters. A crucial factor is certainly the amount of water. We investigate in this work the transport of water from beyond the snow-line to the HZ in a binary star system and compare it to a single star system.

scholarly journals The first magnetic maps of a pre-main-sequence binary star system – HD 155555

2008 ◽  
Vol 387 (2) ◽  
pp. 481-496 ◽  
Author(s):  
N. J. Dunstone ◽  
G. A. J. Hussain ◽  
A. Collier Cameron ◽  
S. C. Marsden ◽  
M. Jardine ◽  
...  
Keyword(s):  
Main Sequence ◽  
Binary Star ◽  
Star System ◽  
Binary Star System

scholarly journals A New Binary Star System of EW Type in Draco: GSC 03905-01870

2018 ◽  
Author(s):  
Salvador Barquin
Keyword(s):  
Light Curve ◽  
Binary Stars ◽  
Variable Star ◽  
Binary Star ◽  
Type I ◽  
Star System ◽  
Primary Minimum ◽  
Eclipsing Binary ◽  
Eclipsing Binary Stars ◽  
Binary Star System

Discovery of a new binary star system (GSC 03905-01870 = USNO-B1.0 1431-0327922 = UCAC4 716-059522) in the Draco constellation is presented. It was discovered during a search for previously unreported eclipsing binary stars through the ASAS-SN database. The shape of the light curve and its characteristics (period of 0.428988±0.000001 d, amplitude of 0.34±0.02 V Mag, primary minimum epoch HJD 2457994.2756±0.0002) indicates that the new variable star is an eclipsing binary of W Ursae Majoris type. I registered this variable star in The International Variable Star Index (VSX), its AAVSO UID is 000-BMP-891.

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