The Impact of Stellar Abundance Variations on Stellar Habitable Zone Evolution

Young, Patrick; Liebst, Kelley; Pagano, Michael

doi:10.1088/2041-8205/755/2/l31

Cited by 34 publications

(11 citation statements)

References 42 publications

(45 reference statements)

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“…Our improvements to MESA star for gas giant planets were motivated by the dramatic growth in this field. Over 800 exoplanets have been confirmed, and their study has prompted enormous progress in our understanding of the formation and migration of giant planets, and of the importance of factors such as stellar mass (Laughlin et al 2004;Alibert et al 2011;Boss 2011), composition (Fischer & Valenti 2005;Young et al 2012), and binarity (Patience et al 2002;Mugrauer & Neuhäuser 2009;Roell et al 2012). Puzzles remain, though, both in our solar system and in the studies of the plethora of these newly discovered exoplanets, including the characteristics of the planet-hosting stars and the interiors, atmospheres, surface gravities, temperatures, and compositions of the planets (e.g., Udry & Santos 2007;Seager & Deming 2010).…”

Section: Mixing Mechanisms Involving Compositionmentioning

confidence: 99%

Modules for Experiments in Stellar Astrophysics (Mesa): Planets, Oscillations, Rotation, and Massive Stars

Paxton

Cantiello

Arras

et al. 2013

ApJS

3,134

3,206

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We substantially update the capabilities of the open source software package Modules for Experiments in Stellar Astrophysics (MESA), and its one-dimensional stellar evolution module, MESA star. Improvements in MESA star's ability to model the evolution of giant planets now extends its applicability down to masses as low as one-tenth that of Jupiter. The dramatic improvement in asteroseismology enabled by the space-based Kepler and CoRoT missions motivates our full coupling of the ADIPLS adiabatic pulsation code with MESA star. This also motivates a numerical recasting of the Ledoux criterion that is more easily implemented when many nuclei are present at non-negligible abundances. This impacts the way in which MESA star calculates semi-convective and thermohaline mixing. We exhibit the evolution of 3-8 M stars through the end of core He burning, the onset of He thermal pulses, and arrival on the white dwarf cooling sequence. We implement diffusion of angular momentum and chemical abundances that enable calculations of rotating-star models, which we compare thoroughly with earlier work. We introduce a new treatment of radiation-dominated envelopes that allows the uninterrupted evolution of massive stars to core collapse. This enables the generation of new sets of supernovae, long gamma-ray burst, and pair-instability progenitor models. We substantially modify the way in which MESA star solves the fully coupled stellar structure and composition equations, and we show how this has improved the scaling of MESA's calculational speed on multi-core processors. Updates to the modules for equation of state, opacity, nuclear reaction rates, and atmospheric boundary conditions are also provided. We describe the MESA Software Development Kit (SDK) that packages all the required components needed to form a unified, maintained, and well-validated build environment for MESA. We also highlight a few tools developed by the community for rapid visualization of MESA star results.

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Section: Mixing Mechanisms Involving Compositionmentioning

confidence: 99%

Modules for Experiments in Stellar Astrophysics (Mesa): Planets, Oscillations, Rotation, and Massive Stars

Paxton

Cantiello

Arras

et al. 2013

ApJS

3,134

3,206

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“…Moreover, for a star with a fixed effective radiating temperature, T eff , stellar luminosity depends on the metallicity of a star (Chabrier & Baraffe 2000;Dotter et al 2008, see Figure 2(a)) because of changes in the opacity of the stellar atmosphere. So the HZ also varies as a function of stellar metallicity (Young et al 2012). In this srudy, we used the Dartmouth stellar evolution database (Dotter et al 2008) 11 to obtain L å and M å for both low ([Fe/H]=−0.5) and high ([Fe/ H]=0.3) metallicities, as a function of T eff .…”

Section: Calculation Of Correct Orbital Periodsmentioning

confidence: 99%

The Inner Edge of the Habitable Zone for Synchronously Rotating Planets Around Low-Mass Stars Using General Circulation Models

Kopparapu

Wolf

Haqq-Misra

et al. 2016

ApJ

212

264

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Terrestrial planets at the inner edge of the habitable zone (HZ) of late-K and M-dwarf stars are expected to be in synchronous rotation, as a consequence of strong tidal interactions with their host stars. Previous global climate model (GCM) studies have shown that, for slowly rotating planets, strong convection at the substellar point can create optically thick water clouds, increasing the planetary albedo, and thus stabilizing the climate against a thermal runaway. However these studies did not use self-consistent orbital/rotational periods for synchronously rotating planets placed at different distances from the host star. Here we provide new estimates of the inner edge of the HZ for synchronously rotating terrestrial planets around late-K and M-dwarf stars using a 3D Earth-analog GCM with self-consistent relationships between stellar metallicity, stellar effective temperature, and the planetary orbital/rotational period. We find that both atmospheric dynamics and the efficacy of the substellar cloud deck are sensitive to the precise rotation rate of the planet. Around mid-to-late M-dwarf stars with low metallicity, planetary rotation rates at the inner edge of the HZ become faster, and the inner edge of the HZ is farther away from the host stars than in previous GCM studies. For an Earth-sized planet, the dynamical regime of the substellar clouds begins to transition as the rotation rate approaches ∼10 days. These faster rotation rates produce stronger zonal winds that encircle the planet and smear the substellar clouds around it, lowering the planetary albedo, and causing the onset of the water-vapor greenhouse climatic instability to occur at up to ∼25% lower incident stellar fluxes than found in previous GCM studies. For mid-to-late M-dwarf stars with high metallicity and for mid-K to early-M stars, we agree with previous studies.

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“…The correlation of gas giant exoplanets with high metallicity host stars supports the core accretion model of planet formation because their primordial disks are expected to have more rocky planetesimals from which the rocky cores of gas giants are formed ). Recently, attention has been given to the effect of metallicity on the habitable zones around cool dwarfs with masses < 0.5 M ⊙ with Kepler Objects of Interest (Muirhead et al 2012) and the effect of abundance ratios of metals other than Fe in the evolution of the habitable zones around 1 M ⊙ stars (Young, Liebst, and Pagano 2012).…”

Section: Introductionmentioning

confidence: 99%

Effect of Metallicity on the Evolution of the Habitable Zone From the Pre-Main Sequence to the Asymptotic Giant Branch and the Search for Life

Danchi

López

2013

ApJ

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During the course of stellar evolution, the location and width of the habitable zone changes as the luminosity and radius of the star evolves. The duration of habitability for a planet located at a given distance from a star is greatly affected by the characteristics of the host star. A quantification of these effects can be used observationally in the search for life around nearby stars. The longer the duration of habitability, the more likely it is that life has evolved. The preparation of observational techniques aimed at detecting life would benefit from the scientific requirements deduced from the evolution of the habitable zone. We present a study of the evolution of the habitable zone around stars of 1.0, 1.5, and 2.0 M ⊙ for metallicities ranging from Z=0.0001 to Z=0.070. We also consider the evolution of the habitable zone from the pre-main sequence until the asymptotic giant branch is reached. We find that metallicity strongly affects the duration of the habitable zone for a planet as well as the distance from the host star where the duration is maximized. For a 1.0 M ⊙ star with near Solar metallicity, Z=0.017, the duration of the habitable zone is >10 Gyr at distances 1.2 to 2.0 AU from

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The Impact of Stellar Abundance Variations on Stellar Habitable Zone Evolution

Cited by 34 publications

References 42 publications

Modules for Experiments in Stellar Astrophysics (Mesa): Planets, Oscillations, Rotation, and Massive Stars

Modules for Experiments in Stellar Astrophysics (Mesa): Planets, Oscillations, Rotation, and Massive Stars

The Inner Edge of the Habitable Zone for Synchronously Rotating Planets Around Low-Mass Stars Using General Circulation Models

Effect of Metallicity on the Evolution of the Habitable Zone From the Pre-Main Sequence to the Asymptotic Giant Branch and the Search for Life

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