The M-dwarfs in Multiples (MinMs) survey – I. Stellar multiplicity among low-mass stars within 15 pc★

Ward-Duong, Kimberly; Patience, J.; Rosa, Robert J. De; Bulger, J.; Rajan, Abhijith; Goodwin, S. P.; Parker, R. J.; McCarthy, Donald W.; Kulesa, Craig

doi:10.1093/mnras/stv384

Cited by 111 publications

(122 citation statements)

References 67 publications

(60 reference statements)

Supporting

Mentioning

103

Contrasting

Order By: Relevance

“…One such possible mechanism involves a significant amount of planet-forming material migrating inwards from more distant regions of a protostellar disk, thereby providing enough mass to build greater numbers of small planets close to their stars, and larger cumulative planetary masses for M-dwarf host stars (Mulders et al, 2015c). And the fraction of lowmass stars with stellar companions (∼23.5%, Ward-Duong et al, 2015) is lower than solar-type stars (>40%, Raghavan et al, 2010), which may reduce the likelihood of protoplanetary disk truncation in M-dwarf systems (Artymowicz & Lubow, 1994).…”

Section: Gravitational Effectsmentioning

confidence: 99%

The habitability of planets orbiting M-dwarf stars

2016

View full text Add to dashboard Cite

The prospects for the habitability of M-dwarf planets have long been debated, due to key differences between the unique stellar and planetary environments around these low-mass stars, as compared to hotter, more luminous Sunlike stars. Over the past decade, significant progress has been made by both space-and ground-based observatories to measure the likelihood of small planets to orbit in the habitable zones of M-dwarf stars. We now know that most M dwarfs are hosts to closely-packed planetary systems characterized by a paucity of Jupiter-mass planets and the presence of multiple rocky planets, with roughly a third of these rocky M-dwarf planets orbiting within the habitable zone, where they have the potential to support liquid water on their surfaces. Theoretical studies have also quantified the effect on climate and habitability of the interaction between the spectral energy distribution of M-dwarf stars and the atmospheres and surfaces of their planets. These and other recent results fill in knowledge gaps that existed at the time of the previous overview papers published nearly a decade ago by Tarter et al. (2007) and Scalo et al. (2007). In this review we provide a comprehensive picture of the current knowledge of M-dwarf planet occurrence and habitability based on work done in this area over the past decade, and summarize future directions planned in this quickly evolving field.

show abstract

Section: Gravitational Effectsmentioning

confidence: 99%

The habitability of planets orbiting M-dwarf stars

2016

View full text Add to dashboard Cite

show abstract

“…The adopted uncertainty for the HARPS absolute radial velocity is 0.5 km/s; (11) Rodriguez et al (2015); (12) Ward-Duong et al (2015); (13) Kopparapu et al (2013Kopparapu et al ( , 2014; (14) Kopparapu et al (2016) activity. We also measure from the spectra the chromospheric emission in the Ca ii H&K lines, and in the Hα, Hβ, Hγ, and Na D lines (Wilson 1968;Giampapa et al 1978;Linsky et al 1982).…”

Section: Spectroscopic Indicesmentioning

confidence: 99%

The HARPS search for southern extra-solar planets

Astudillo-Defru

Forveille

Bonfils

et al. 2017

A&A

132

View full text Add to dashboard Cite

Context. Low-mass stars are currently the best targets when searching for rocky planets in the habitable zone of their host star. Over the last 13 years, precise radial velocities measured with the HARPS spectrograph have identified over a dozen super-Earths and Earth-mass planets (msin i ≤ 10 M ⊕ ) around M dwarfs, with a well-understood selection function. This well-defined sample provides information on their frequency of occurrence and on the distribution of their orbital parameters, and therefore already constrains our understanding of planetary formation. The subset of these low-mass planets that were found within the habitable zone of their host star also provide prized targets for future searches of atmospheric biomarkers. Aims. We are working to extend this planetary sample to lower masses and longer periods through dense and long-term monitoring of the radial velocity of a small M dwarf sample. Methods. We obtained large numbers of HARPS spectra for the M dwarfs GJ 3138, GJ 3323, GJ 273, GJ 628, and GJ 3293, from which we derived radial velocities (RVs) and spectroscopic activity indicators. We searched for variabilities, periodicities, Keplerian modulations, and correlations, and attribute the radial-velocity variations to combinations of planetary companions and stellar activity. Results. We detect 12 planets, 9 of which are new with masses ranging from 1.17 to 10.5 M ⊕ . These planets have relatively short orbital periods (P<40 d), except for two that have periods of 217.6 and 257.8 days. Among these systems, GJ 273 harbor two planets with masses close to the Earth's. With a distance of only 3.8 parsec, GJ 273 is the second nearest known planetary system -after Proxima Centauri -with a planet orbiting the circumstellar habitable zone.

show abstract

“…While it has been shown that stellar companions are less common around M dwarfs than around more massive stars (Henry 1991;Fischer & Marcy 1992;Duchêne & Kraus 2013;Janson et al 2014;Ward-Duong et al 2015;Winters 2015), brown dwarf companions to M dwarfs are even more rare. Few examples are known, despite significant efforts to identify them in the solar neighborhood (Campbell et al 1988;Marcy & Benitz 1989;Henry & McCarthy 1990;Tokovinin 1992;Dieterich et al 2012).…”

Section: Introductionmentioning

confidence: 99%

LHS 1610A: A Nearby Mid-M Dwarf with a Companion That Is Likely a Brown Dwarf

Winters

Irwin

Newton

et al. 2018

View full text Add to dashboard Cite

We present the spectroscopic orbit of LHS1610A, a newly discovered single-lined spectroscopic binary with a trigonometric distance placing it at 9.9±0.2 pc. We obtained spectra with the TRES instrument on the 1.5 m Tillinghast Reflector at the Fred Lawrence Whipple Observatory located on Mt. Hopkins in AZ. We demonstrate the use of the TiO molecular bands at 7065-7165Åto measure radial velocities and achieve an average estimated velocity uncertainty of 28 m s −1 . We measure the orbital period to be 10.6 days and calculate a minimum mass of 44.8±3.2 M Jup for the secondary, indicating that it is likely a brown dwarf. We place an upper limit to 3σ of 2500 K on the effective temperature of the companion from infrared spectroscopic observations using IGRINS on the 4.3 m Discovery Channel Telescope. In addition, we present a new photometric rotation period of 84.3 days for the primary star using data from the MEarth-South Observatory, with which we show that the system does not eclipse.

show abstract

The M-dwarfs in Multiples (MinMs) survey – I. Stellar multiplicity among low-mass stars within 15 pc★

Cited by 111 publications

References 67 publications

The habitability of planets orbiting M-dwarf stars

The habitability of planets orbiting M-dwarf stars

The HARPS search for southern extra-solar planets

LHS 1610A: A Nearby Mid-M Dwarf with a Companion That Is Likely a Brown Dwarf

Contact Info

Product

Resources

About