Detailed abundances of planet-hosting wide binaries. II. HD 80606+HD 80607

Journal Article · Wed Feb 10 04:00:00 EST 2016 · Astrophysical Journal

DOI:https://doi.org/10.3847/0004-637X/818/1/54· OSTI ID:22887052

Mack, III, Claude E.; Stassun, Keivan G. ^[1]; Schuler, Simon C. ^[2]; Hebb, Leslie ^[3]

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1. Vanderbilt University, Department of Physics and Astronomy, Nashville, TN 37235 (United States)
2. University of Tampa, Department of Chemistry, Biochemistry, and Physics, Tampa, FL 33606 (United States)
3. Hobart and William Smith Colleges, Department of Physics, Geneva, NY 14456 (United States)

We present a detailed chemical abundance analysis of 15 elements in the planet-hosting wide binary (PHWB) system HD 80606+HD 80607 using Keck/HIRES spectra. As in our previous analysis of the PHWB HD 20782+HD 20781, we presume that these two G5 dwarf stars formed together and therefore had identical primordial abundances. In this binary, HD 80606 hosts an eccentric (e≈0.93) giant planet at ∼0.5 AU, but HD 80607 has no detected planets. If close-in giant planets on eccentric orbits are efficient at scattering rocky planetary material into their host stars, then HD 80606 should show evidence of having accreted rocky material while HD 80607 should not. Here we show that the trends of abundance versus element condensation temperature for HD 80606 and HD 80607 are statistically indistinguishable, corroborating the recent result of Saffe et al. This could suggest that both stars accreted similar amounts of rocky material; indeed, our model for the chemical signature of rocky planet accretion indicates that HD 80606 could have accreted up to 2.5 M{sub ⊕} of rocky material—about half that contained in the Solar System and primordial asteroid belt—relative to HD 80607 and still be consistent with the data. Since HD 80607 has no known giant planets that might have pushed rocky planet material via migration onto that star, we consider it more likely that HD 80606/07 experienced essentially no rocky planet accretion. This in turn suggests that the migration history of the HD 80606 giant planet must have been such that it ejected any close-in planetary material that might have otherwise been shepherded onto the star.

• OSTI ID: 22887052
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 818; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United Kingdom
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
ASTEROIDS
DWARF STARS
ELEMENT ABUNDANCE
MIGRATION
PLANETS
SCATTERING
SPECTRA