Exploring the Frequency of Close-in Jovian Planets around M Dwarfs

By M. Endl, W. Cochran, M. Kuerster, D. Paulson, R. Wittenmyer, P. MacQueen, R. Tull. 2006

165 citations recorded by the source corpus.

We discuss our high-precision radial velocity results of a sample of 90 M dwarfs observed with the Hobby-Eberly Telescope and the Harlan J. Smith 2.7 m Telescope at McDonald Observatory, as well as the ESO VLT and the Keck I telescopes, within the context of the overall frequency of Jupiter-mass planetary companions to main-sequence stars. None of the stars in our sample show variability indicative of a giant planet in a short-period orbit, with a ≤ 1 AU. We estimate an upper limit of the frequency f of close-in Jovian planets around M dwarfs as <1.27% (at the 1 σ confidence level). Furthermore, we determine that the efficiency of our survey in noticing planets in circular orbits is 98% for companions with m sin i > 3.8MJ and a ≤ 0.7 AU. For eccentric orbits (e = 0.6) the survey completeness is 95% for all planets with m sin i > 3.5MJ and a ≤ 0.7 AU. Our results point toward a generally lower frequency of close-in Jovian planets for M dwarfs as compared to FGK-type stars. This is an important piece of information for our understanding of the process of planet formation as a function of stellar mass.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/7875f53b4b88400beed8334edacd28c45892c623

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In Astronomy and Astrophysics

1. J. Johnson
2. D. Charbonneau
3. Nuno C. Santos
4. J. Winn
5. Debra A. Fischer
6. M. Mayor
7. J. Southworth
8. S. Udry

Citations in the corpus

• THE NIRSPEC ULTRACOOL DWARF RADIAL VELOCITY SURVEY (2010, methodology): “While it has been shown that early M dwarfs have a relative paucity of close in Jupiter-mass planets (Endl et al. 2006; Johnson et al. 2007), we are just now beginning to understand the occurrence of superEarth (Mp < 10 M⊕) planets to mid-M stars or any type of planet orbiting late-M or L dwarfs.”
• Spectroscopic parameters for 451 stars in the HARPS GTO planet search program - Stellar [Fe/H] and the frequency of exo-Neptunes (2008, background): “It has been proposed that M-dwarf stars may have a lower rate of Jupiter-like planets,but (at least in the short planet period range) a high incidence of Neptune-like planet detections (Endl et al. 2006; Bonfils etal.”
• 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 HARPS search for southern extra-solar planets - XXXI. The M-dwarf sample (2011, background): “E P] 2 3 N ov 2 X. Bonfils et al.: The HARPS M-dwarf sample sun-like stars (Bonfils et al. 2006; Butler et al. 2004; Endl et al. 2006; Johnson et al. 2007; Cumming et al. 2008).”
• Planets around evolved intermediate-mass stars - I. Two substellar companions in the open clusters NGC 2423 and NGC 4349 (2007, methodology): “Precise RV surveys targeting the first two bins have been ongoing for more than a decade and have yielded reliable estimates of giant planet frequency around solar-type stars (Udry et al. 2007; Marcy et al. 2006) and M dwarfs (Bonfils et al. 2006; Endl et al. 2006; Butler et al. 2006).”
• The Keck Planet Search: Detectability and the Minimum Mass and Orbital Period Distribution of Extrasolar Planets (2008, background): “…in the core accretion scenario for planet formation (Laughlin, Bodenheimer, & Adams 2004; Ida & Lin 2005; Kennedy & Kenyon 2008 although see Kornet & Wolf 2006), and observational estimates support this picture (Butler et al. 2004b; Butler et al. 2006b; Endl et al. 2006; Johnson et al. 2007).”
• THE SOLAR NEIGHBORHOOD. XXXVII. THE MASS–LUMINOSITY RELATION FOR MAIN-SEQUENCE M DWARFS (2016, methodology): “Treating GJ 623 AB as a single lined spectroscopic binary, we obtained from the CE and from the HET (Endl et al. 2006) velocities for component A at most orbital phases, as shown in the right panel of Figure 10.”
• SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs - I. New atmospheric parameters and masses for 48 stars with planets (2013, background): “Iis now widely accepted that the frequency of giant planets orbiting (lower mass) M-dwarfs is considerably lower than the one found for FGK dwarfs (Bonfils et al. 2005b, 2011; Endl et al. 2006), at least regarding the short period domain (Neves et al. 2013).”
• PLANETS AROUND LOW-MASS STARS (PALMS). IV. THE OUTER ARCHITECTURE OF M DWARF PLANETARY SYSTEMS (2014, background): “This well-established trend between planet occurrence 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…”
• A Decreased Probability of Habitable Planet Formation around Low-Mass Stars (2007, background): “2004; Fischer & Valenti 2005) allow for 70-90% of stars to have planetary systems without Jovians, and an even larger fraction for lower-mass stars (Endl et al. 2006; Butler et al. 2006).”
• The HARPS search for southern extra-solar planets. X. A m sin i = 11 M_â planet around the nearby spotted M dwarf GJ 674 (2007, background): “To date, none of the ∼300 M dwarfs scrutinized for planets by the various radial-velocity searches (Bonfils et al. 2006; Endl et al. 2006; Butler et al. 2006) has been found to host a hot Jupiter.”
• TEN NEW AND UPDATED MULTIPLANET SYSTEMS AND A SURVEY OF EXOPLANETARY SYSTEMS (2008, background): “This trend, if it is not simply Poisson noise and should hold up as more M-dwarf systems are discovered, is especially surprising since M dwarfs have a lower-than-average planet occurrence rate (Endl et al. 2006; Johnson et al. 2007a; Mayor et al. 2008).”
• New companions to nearby low-mass stars (2013, unknown): “…B M0 2008-08-25 2078 47.7 ± 0.4 61 ± 3 6.22 Gl 856 A M3V 2008-07-14 1484 50.0 ± 0.5 24 ± 4 1.21 (Zuckerman, Song & Bessell 2004) Gl 863.1 A K5 2008-08-24 662 275.7 ± 1.1 16.2 ± 2.4 0.73 (Hartkopf et al. 2000) Gl 864 M1V 2008-08-25 653 237.1 ± 1.2 11.5 ± 0.4 3.43 (Endl et al. 2006) Gl 893.4 M0.”
• THE OCCURRENCE RATE OF SMALL PLANETS AROUND SMALL STARS (2013, result): “…low occurrence rate of giant planets is consistent with previous estimates of the giant planet occurrence rate around cool stars (Butler et al. 2004; Bonfils et al. 2006; Butler et al. 2006; Endl et al. 2006; Johnson et al. 2007; Cumming et al. 2008; Bonfils et al. 2011; Howard et al. 2012).”
• The Occurrence and Architecture of Exoplanetary Systems (2014, background): “One secure result is that they have fewer giant planets with P <∼ 1 yr than FGK dwarfs (Butler et al. 2004, Endl et al. 2006, Johnson et al. 2007, Bonfils et al. 2013).”