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ON THE AGE OF GLIESE 86
Gliese 86 is a nearby planet hosting a visual binary consisting of a K-type primary, G1 86 A, and a white dwarf secondary, G1 86 B. In this work, we present a model atmosphere analysis of the M sub(A) = 0.83 M sub([middot in circle]) primary, whose chemistry unambiguously identifies it as a 10 Gyr o...
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Published in: | The Astrophysical journal 2014-04, Vol.785 (1), p.1-4, Article 68 |
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description | Gliese 86 is a nearby planet hosting a visual binary consisting of a K-type primary, G1 86 A, and a white dwarf secondary, G1 86 B. In this work, we present a model atmosphere analysis of the M sub(A) = 0.83 M sub([middot in circle]) primary, whose chemistry unambiguously identifies it as a 10 Gyr old disk star. For the secondary, this gives rise to a progenitor mass M sub(prog) = 1.11 + or - 0.05 M sub([middot in circle]), and-by inference with its local sibling o super(2) Eri-a white dwarf mass M sub(B) = 0.49 + or - 0.02 M sub([middot in circle]). The discrepancy with the 2-3 Gyr chromospheric age of G1 86 A, as first noted by Rocha-Pinto, Castilho & Maciel, is thus most plausibly the result of a former accretion of mass and angular momentum from the distant degenerate. In consequence, this also implies that with respect to shorter-period systems, like Sirius or Procyon, one must expect significant wind accretion when they evolve through the planetary nebula phase, such that the system ages cannot be reliably determined from their currently bright primaries. |
doi_str_mv | 10.1088/0004-637X/785/1/68 |
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In this work, we present a model atmosphere analysis of the M sub(A) = 0.83 M sub([middot in circle]) primary, whose chemistry unambiguously identifies it as a 10 Gyr old disk star. For the secondary, this gives rise to a progenitor mass M sub(prog) = 1.11 + or - 0.05 M sub([middot in circle]), and-by inference with its local sibling o super(2) Eri-a white dwarf mass M sub(B) = 0.49 + or - 0.02 M sub([middot in circle]). The discrepancy with the 2-3 Gyr chromospheric age of G1 86 A, as first noted by Rocha-Pinto, Castilho & Maciel, is thus most plausibly the result of a former accretion of mass and angular momentum from the distant degenerate. 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In this work, we present a model atmosphere analysis of the M sub(A) = 0.83 M sub([middot in circle]) primary, whose chemistry unambiguously identifies it as a 10 Gyr old disk star. For the secondary, this gives rise to a progenitor mass M sub(prog) = 1.11 + or - 0.05 M sub([middot in circle]), and-by inference with its local sibling o super(2) Eri-a white dwarf mass M sub(B) = 0.49 + or - 0.02 M sub([middot in circle]). The discrepancy with the 2-3 Gyr chromospheric age of G1 86 A, as first noted by Rocha-Pinto, Castilho & Maciel, is thus most plausibly the result of a former accretion of mass and angular momentum from the distant degenerate. In consequence, this also implies that with respect to shorter-period systems, like Sirius or Procyon, one must expect significant wind accretion when they evolve through the planetary nebula phase, such that the system ages cannot be reliably determined from their currently bright primaries.</abstract><cop>United States</cop><doi>10.1088/0004-637X/785/1/68</doi><tpages>4</tpages><orcidid>https://orcid.org/0000-0002-1355-9802</orcidid><oa>free_for_read</oa></addata></record> |
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subjects | Accretion Age ANGULAR MOMENTUM ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ATMOSPHERES BINARY STARS Disks MASS TRANSFER PLANETARY NEBULAE PLANETS Procyon Progenitors (astrophysics) STELLAR WINDS Visual WHITE DWARF STARS |
title | ON THE AGE OF GLIESE 86 |
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