A minimum mass nebula for M dwarfs

Gaidos, Eric

doi:10.1093/mnrasl/slx063

Cited by 47 publications

(20 citation statements)

References 41 publications

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“…While the solids in giant planets and protoplanetary disks show a positive scaling with stellar mass, this relation breaks down for sub-Neptunes at short orbital periods. The estimated amount of solids in M dwarf planetary systems is higher than that in sun-like stars (Mulders et al 2015c;Gaidos 2017), reflecting the trend in planet occurrence.…”

Section: Low Mass Starsmentioning

confidence: 88%

“…Radial redistribution of material likely plays a role, as illustrated in Figure 8. There is some evidence in the exoplanet population that the solid distribution in M dwarf disk may have been more centrally peaked than for sun-like stars (Gaidos 2017), perhaps reflecting more efficient radial drift of dust around low-mass stars (Pinilla et al 2013). Besides disk mass, the lower luminosity of less massive stars (both on the main sequence and pre-main-sequence) means that disk are cooler than their counterparts around higher mass stars.…”

Section: Low Mass Starsmentioning

confidence: 99%

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Planet Populations as a Function of Stellar Properties

Mulders

2018

Handbook of Exoplanets

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Exoplanets around different types of stars provide a window into the diverse environments in which planets form. This chapter describes the observed relations between exoplanet populations and stellar properties and how they connect to planet formation in protoplanetary disks. Giant planets occur more frequently around more metal-rich and more massive stars. These findings support the core accretion theory of planet formation, in which the cores of giant planets form more rapidly in more metal-rich and more massive protoplanetary disks. Smaller planets, those with sizes roughly between Earth and Neptune, exhibit different scaling relations with stellar properties. These planets are found around stars with a wide range of metallicities and occur more frequently around lower mass stars. This indicates that planet formation takes place in a wide range of environments, yet it is not clear why planets form more efficiently around low mass stars. Going forward, exoplanet surveys targeting M dwarfs will characterize the exoplanet population around the lowest mass stars. In combination with ongoing stellar characterization, this will help us understand the formation of planets in a large range of environments.

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Section: Low Mass Starsmentioning

confidence: 88%

Section: Low Mass Starsmentioning

confidence: 99%

Planet Populations as a Function of Stellar Properties

Mulders

2018

Handbook of Exoplanets

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“…To date, there remain only a few disks detected around M stars. Whether this is due to the poorer sensitivity in terms of fractional luminosity for M stars (see Morey & Lestrade 2014, and references therein) or different progenitor properties (e.g., Gaidos 2017) is not yet resolved. The current detection rates are typically in the range of a few percent.…”

Section: Demographics: Detecting Debris Disksmentioning

confidence: 99%

Debris Disks: Structure, Composition, and Variability

Hughes

Duchêne

Matthews

2018

Annu. Rev. Astron. Astrophys.

308

327

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Debris disks are tenuous, dust-dominated disks commonly observed around stars over a wide range of ages. Those around main sequence stars are analogous to the Solar System's Kuiper Belt and Zodiacal light. The dust in debris disks is believed to be continuously regenerated, originating primarily with collisions of planetesimals. Observations of debris disks provide insight into the evolution of planetary systems; the composition of dust, comets, and planetesimals outside the Solar System; as well as placing constraints on the orbital architecture and potentially the masses of exoplanets that are not otherwise detectable. This review highlights recent advances in multiwavelength, high-resolution scattered light and thermal imaging that have revealed a complex and intricate diversity of structures in debris disks, and discusses how modeling methods are evolving with the breadth and depth of the available observations. Two rapidly advancing subfields highlighted in this review include observations of atomic and molecular gas around main sequence stars, and variations in emission from debris disks on very short (days to years) timescales, providing evidence of non-steady state collisional evolution particularly in young debris disks.

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“…The detection of planets orbiting these stars is therefore important to constrain the population of planets and the formation processes in the lessmassive protoplanetary disks (Gaidos 2017). Additionally, lowmass and small-sized M dwarfs have advantages when searching for the lowest-mass and smallest-sized planets: the radial velocity (RV) amplitude and transit depth scales with M −2/3 and R −2 , respectively.…”

Section: Introductionmentioning

confidence: 99%

The HARPS search for southern extra-solar planets

Astudillo-Defru

Díaz

Bonfils

et al. 2017

A&A

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Exoplanet surveys have shown that systems with multiple low-mass planets on compact orbits are common. Except for a few cases, however, the masses of these planets are generally unknown. At the very end of the main sequence, host stars have the lowest mass and hence offer the largest reflect motion for a given planet. In this context, we monitored the low-mass (0.13 M ) M dwarf YZ Cet (GJ 54.1, HIP 5643) intensively and obtained radial velocities and stellar-activity indicators derived from spectroscopy and photometry, respectively. We find strong evidence that it is orbited by at least three planets in compact orbits (P Orb = 1.97, 3.06, 4.66 days), with the inner two near a 2:3 mean-motion resonance. The minimum masses are comparable to the mass of Earth (M sin i = 0.75 ± 0.13, 0.98 ± 0.14, and 1.14 ± 0.17 M ⊕ ), and they are also the lowest masses measured by radial velocity so far. We note the possibility for a fourth planet with an even lower mass of M sin i = 0.472 ± 0.096 M ⊕ at P Orb = 1.04 days. An n-body dynamical model is used to place further constraints on the system parameters. At 3.6 parsecs, YZ Cet is the nearest multi-planet system detected to date.

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A minimum mass nebula for M dwarfs

Cited by 47 publications

References 41 publications

Planet Populations as a Function of Stellar Properties

Planet Populations as a Function of Stellar Properties

Debris Disks: Structure, Composition, and Variability

The HARPS search for southern extra-solar planets

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