RETIRED A STARS AND THEIR COMPANIONS. III. COMPARING THE MASS–PERIOD DISTRIBUTIONS OF PLANETS AROUND A-TYPE STARS AND SUN-LIKE STARS

By B. Bowler, J. Johnson, G. Marcy, G. Henry, K. Peek, Debra A. Fischer, K. Clubb, Michael C. Liu, S. Reffert, C. Schwab and 1 more. 2009

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We present an analysis of ∼5 years of Lick Observatory radial velocity measurements targeting a uniform sample of 31 intermediate-mass (IM) subgiants (1.5 ≲ M*/M☉≲ 2.0) with the goal of measuring the occurrence rate of Jovian planets around (evolved) A-type stars and comparing the distributions of their orbital and physical characteristics to those of planets around Sun-like stars. We provide updated orbital solutions incorporating new radial velocity measurements for five known planet-hosting stars in our sample; uncertainties in the fitted parameters are assessed using a Markov-Chain Monte Carlo method. The frequency of Jovian planets interior to 3 AU is 26+9−8%, which is significantly higher than the 5%–10% frequency observed around solar-mass stars. The median detection threshold for our sample includes minimum masses down to {0.2, 0.3, 0.5, 0.6, 1.3} MJup within {0.1, 0.3, 0.6, 1.0, 3.0} AU. To compare the properties of planets around IM stars to those around solar-mass stars we synthesize a population of planets based on the parametric relationship dN ∝ MαPβdlnMdlnP, the observed planet frequency, and the detection limits we derived. We find that the values of α and β for planets around solar-type stars from Cumming et al. fail to reproduce the observed properties of planets in our sample at the 4σ level, even when accounting for the different planet occurrence rates. Thus, the properties of planets around A stars are markedly different than those around Sun-like stars, suggesting that only a small (∼50%) increase in stellar mass has a large influence on the formation and orbital evolution of planets.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/553f193d9e149d82c09b11169f6a7bc631a85fa7

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THE LICK-CARNEGIE EXOPLANET SURVEY: A URANUS-MASS FOURTH PLANET FOR GJ 876 IN AN EXTRASOLAR LAPLACE CONFIGURATION (2010, background): “During the past decade, both of these trends have been established observationally (see, e.g., Fischer & Valenti 2005 for a discussion of the metallicity trend and Johnson et al. 2008 and Bowler et al. 2010 for discussions of the mass trend.)”
THE FALSE POSITIVE RATE OF KEPLER AND THE OCCURRENCE OF PLANETS (2013, result): “Indeed, the results from the study of planets orbiting A-type stars by Bowler et al. (2010) provides an explanation for the apparent discrepancy between RV and Kepler results for the occurrence of giant planets orbiting hot stars: Figure 1 of the above paper shows that no Doppler planets have been…”
The frequency of planetary debris around young white dwarfs (2014, background): “While there have been a number of planet detections, there is an intense ongoing debate regarding the true masses of subgiant planet hosts (Bowler et al. 2010; Johnson et al. 2010, 2013; Lloyd 2013, 2011).”
An ALMA Survey of Protoplanetary Disks in the σ Orionis Cluster (2017, background): “…Andrews et al. 2013) revealed a positive dependence between disk dust mass (Mdust) and host star mass (M∗), which could fundamentally explain the positive correlation between giant planet frequency and stellar mass (Endl et al. 2006; Johnson et al. 2007; Bowler et al. 2010; Bonfils et al. 2013).”
THE IMPACT OF STELLAR MULTIPLICITY ON PLANETARY SYSTEMS. I. THE RUINOUS INFLUENCE OF CLOSE BINARY COMPANIONS (2016, background): “…nearly 1000 confirmed planets around other stars (Wright et al. 2011) and thousands of additional candidates (Borucki et al. 2010; Batalha et al. 2013; Burke et al. 2014), revolutionizing the demography of planetary systems (e.g., Fischer & Valenti 2005; Bowler et al. 2010; Johnson et al. 2010).”
Imaging Extrasolar Giant Planets (2016, background): “…massive stars analogous to the well-established correlation at small separations (Johnson et al. 2007; Lovis & Mayor 2007; Johnson et al. 2010; Bowler et al. 2010b), this trend is not yet statistically significant at wide orbital distances and requires larger sample sizes in each stellar mass…”
Extrasolar planet population synthesis - IV. Correlations with disk metallicity, mass, and lifetime (2012, background): “(5) Giant planets are more frequently found orbiting A stars than orbiting solar-like stars, and are also more massive (Lovis & Mayor 2007; Bowler et al. 2010) on average.”
TERRESTRIAL PLANET OCCURRENCE RATES FOR THE KEPLER GK DWARF SAMPLE (2015, background): “…8 BAERI/NASA Ames Research Center, Moffett Field, CA 94035, USA 2005; Naef et al. 2005; Gould et al. 2006; Sahu et al. 2006; Cumming et al. 2008; Bowler et al. 2010; Howard et al. 2010; Bayliss & Sackett 2011; Mayor et al. 2011; van Saders & Gaudi 2011; Wright et al. 2012; Bonfils et al. 2013;…”
THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS (2013, background): “The observational demographics of the exoplanet population strongly support this latter core accretion scenario: the incidence of giant planets orbiting <2.5AU from their hosts scales roughly linearly with M∗ (e.g., Johnson et al. 2007, 2010; Bowler et al. 2010).”
ANCIENT PLANETARY SYSTEMS ARE ORBITING A LARGE FRACTION OF WHITE DWARF STARS (2010, background): “For example, from a study of post-main sequence giant stars, Bowler et al. (2010) report that 1/4 or more of intermediate mass, main sequence, stars have massive planetary companions within 3 AU.”
ALMA SURVEY OF LUPUS PROTOPLANETARY DISKS. I. DUST AND GAS MASSES (2016, background): “…and M∗ in Lupus supports the suggestion by Andrews et al. (2013) that such a relation fundamentally explains the correlation between giant planet frequency and host star mass identified in the exoplanet population (Endl et al. 2006; Johnson et al. 2007; Bonfils et al. 2013; Bowler et al. 2010).”
FORETELLINGS OF RAGNARÖK: WORLD-ENGULFING ASYMPTOTIC GIANTS AND THE INHERITANCE OF WHITE DWARFS (2012, background): “…Red Giant Branch (RGB) stars has received much attention, since many planets have been discovered around sub-giant, RGB and horizontal branch stars (e.g., Niedzielski et al. 2009; Bowler et al. 2010; Johnson et al. 2011; Wittenmyer et al. 2011; a recent compendium is given in Gettel et al. 2012).”
HOT STARS WITH HOT JUPITERS HAVE HIGH OBLIQUITIES (2010, background): “…not obvious why these mechanisms would have a strong dependence on stellar mass or temperature, although it is interesting that 1.3M⊙ is approximately the same stellar mass above which giant planets are found to have larger masses, wider orbits, and a higher rate of occurrence (Bowler et al. 2010).”
Homogeneous studies of transiting extrasolar planets - III. Additional planets and stellar models (2010, background): “24) shows a much larger scatter in the planet properties, but also that systematic er- not been neglecting ones more massive than this; see Gallandet al. (2005), Johnson et al. (2007) Lagrange et al. (2009) and Bowler et al.(2010). rors are much less important for these objects.”
PLANET OCCURRENCE WITHIN 0.25 AU OF SOLAR-TYPE STARS FROM KEPLER (2011, background): “However, most of these planets orbit at ∼1–2 AU, with almost no planets inside of P = 50 day orbits (Bowler et al. 2010).”
PLANETS AROUND LOW-MASS STARS (PALMS). IV. THE OUTER ARCHITECTURE OF M DWARF PLANETARY SYSTEMS (2014, background): “…rate and stellar host mass (Butler et al. 2004; Endl et al. 2006; Butler et al. 2006; Johnson et al. 2007; Lovis & Mayor 2007; Cumming et al. 2008; Bowler et al. 2010; Bonfils et al. 2013; Gaidos et al. 2013) lends support to the core accretion plus migration model of planet formation (Pollack et…”