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Title: THE OCCURRENCE OF WIDE-ORBIT PLANETS IN BINARY STAR SYSTEMS

Abstract

The occurrence of planets in binary star systems has been investigated via a variety of techniques that sample a wide range of semi-major axes, but with a preponderance of such results applicable to planets with semi-major axes less than a few astronomical units. We utilize a new method—the presence or absence of heavy elements in the atmospheres of white dwarf stars—to elucidate the frequency in main sequence binary star systems of planets with semi-major axes greater than a few astronomical units. We consider only binaries where a putative planetary system orbits one member (no circumbinary planets). For main sequence binaries where the primary star is of spectral type A or F, data in the published literature suggests that the existence of a secondary star with a semi-major axis less than about 1000 AU suppresses the formation and/or long-term stability of an extended planetary system around the primary. For these spectral types and initial semi-major axis ≥1000 AU, extended planetary systems appear to be as common around stars in binary systems as they are around single stars.

Authors:
 [1]
  1. Department of Physics and Astronomy, University of California, Los Angeles, CA 90095 (United States)
Publication Date:
OSTI Identifier:
22365279
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal Letters; Journal Volume: 791; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BINARY STARS; MAIN SEQUENCE STARS; ORBITS; PLANETARY ATMOSPHERES; PLANETS; STABILITY; STELLAR ATMOSPHERES; WHITE DWARF STARS

Citation Formats

Zuckerman, B., E-mail: ben@astro.ucla.edu. THE OCCURRENCE OF WIDE-ORBIT PLANETS IN BINARY STAR SYSTEMS. United States: N. p., 2014. Web. doi:10.1088/2041-8205/791/2/L27.
Zuckerman, B., E-mail: ben@astro.ucla.edu. THE OCCURRENCE OF WIDE-ORBIT PLANETS IN BINARY STAR SYSTEMS. United States. doi:10.1088/2041-8205/791/2/L27.
Zuckerman, B., E-mail: ben@astro.ucla.edu. Wed . "THE OCCURRENCE OF WIDE-ORBIT PLANETS IN BINARY STAR SYSTEMS". United States. doi:10.1088/2041-8205/791/2/L27.
@article{osti_22365279,
title = {THE OCCURRENCE OF WIDE-ORBIT PLANETS IN BINARY STAR SYSTEMS},
author = {Zuckerman, B., E-mail: ben@astro.ucla.edu},
abstractNote = {The occurrence of planets in binary star systems has been investigated via a variety of techniques that sample a wide range of semi-major axes, but with a preponderance of such results applicable to planets with semi-major axes less than a few astronomical units. We utilize a new method—the presence or absence of heavy elements in the atmospheres of white dwarf stars—to elucidate the frequency in main sequence binary star systems of planets with semi-major axes greater than a few astronomical units. We consider only binaries where a putative planetary system orbits one member (no circumbinary planets). For main sequence binaries where the primary star is of spectral type A or F, data in the published literature suggests that the existence of a secondary star with a semi-major axis less than about 1000 AU suppresses the formation and/or long-term stability of an extended planetary system around the primary. For these spectral types and initial semi-major axis ≥1000 AU, extended planetary systems appear to be as common around stars in binary systems as they are around single stars.},
doi = {10.1088/2041-8205/791/2/L27},
journal = {Astrophysical Journal Letters},
number = 2,
volume = 791,
place = {United States},
year = {Wed Aug 20 00:00:00 EDT 2014},
month = {Wed Aug 20 00:00:00 EDT 2014}
}