The impact of M dwarf stellar convection on exoplanetary atmospheric signatures. A 3D radiation-hydrodynamics simulation analysis for high-resolution spectroscopy
Authors: A. Chiavassa, M. Brogi, T. Masseron, R. Van den Broeck, L. Bigot, V. Parmentier
Abstract
M dwarf stars represent prime targets for the detection and characterization of small, temperate exoplanets; however, their complex activity and convective surfaces pose significant challenges for high-resolution spectroscopic studies. This work aims to investigate the impact of stellar convection on high-resolution spectroscopic observations of M dwarf stars and develop an integrated approach combining 3D radiative hydrodynamical simulations, spectroscopic modeling, and transit analysis to mitigate stellar noise. We employ 3D radiative hydrodynamical simulations of M dwarf stellar convection to generate synthetic spectra. We compare the synthetic spectra to actual observations of GJ 3470. We model a high-resolution transit sequence of the Neptune-size GJ 3470 b, including centre-to-limb variations (CLVs) and the Rossiter-McLaughlin effect (RME), and process the sequence via principal component analysis (PCA) to de-trend stellar effects. Comparison of synthetic spectra with actual observations shows that current H2O line lists remain inaccurate, with modest agreement in line strength and position for the chosen K-band interval. During the transit of GJ 3470 b, the amplitude of CLVs+RME is comparable to exoplanet signals. Current PCA can in principle de-trend such effects, but its behaviour is highly dependent on the copresence of telluric and planetary signals. While we are able to correctly detect the exoplanet with no evident bias from stellar residuals, this result is limited to a narrow spectral interval and a specific orbital configuration. This study demonstrates that 3D radiative hydrodynamical simulations are essential for accurately modeling convection-induced spectral variability in M dwarfs. Our integrated framework establishes a foundation to obtain unbiased measurements from future ELT observations of exoplanets orbiting M dwarfs.
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The paper models the Rossiter–McLaughlin effect by recovering the spatially resolved stellar spectrum during transit, while the focal paper simulates its spectral impact and applies PCA.
Abstract
When a planet transits its host star, it blocks regions of the stellar surface from view; this causes a distortion of the spectral lines and a change in the line-of-sight (LOS) velocities, known as the Rossiter-McLaughlin (RM) effect. Since the LOS velocities depend, in part, on the stellar rotation, the RM waveform is sensitive to the star-planet alignment (which provides information on the system's dynamical history). We present a new RM modelling technique that directly measures the spatially-resolved stellar spectrum behind the planet. This is done by scaling the continuum flux of the (HARPS) spectra by the transit light curve, and then subtracting the in- from the out-of-transit spectra…
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The paper tests PCA detrending metrics for near-infrared transmission spectra, while the focal paper examines PCA’s ability to remove convection-related stellar signals alongside telluric and planetary signals.
Abstract
Ground-based high-resolution transmission spectroscopy has emerged as a promising technique for detecting chemicals in transiting exoplanetary atmospheres. Despite chemical inferences in several exoplanets and previous robustness studies, a robust and consistent detrending method to remove telluric and stellar features from transmission spectra has yet to be agreed upon. In this work we investigate the robustness of metrics used to optimise PCA-based detrending for high-resolution transmission spectra of exoplanets in the near-infrared. As a case study, we consider observations of the hot Jupiter HD 189733 b obtained using the CARMENES spectrograph on the 3.5 m CAHA telescope. We confirm tha…
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The paper tests core-accretion models against the observed population of planets around M dwarfs, rather than studying stellar spectral contamination during atmospheric observations.
Abstract
Planet formation is sensitive to the conditions in protoplanetary disks, for which scaling laws as a function of stellar mass are known. We aim to test whether the observed population of planets around low-mass stars can be explained by these trends, or if separate formation channels are needed. We address this question by confronting a state-of-the-art planet population synthesis model with a sample of planets around M dwarfs observed by the HARPS and CARMENES radial velocity (RV) surveys. To account for detection biases, we performed injection and retrieval experiments on the actual RV data to produce synthetic observations of planets that we simulated following the core accretion paradigm…
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The paper investigates correcting stellar contamination in exoplanet transmission spectra, while the focal paper models M-dwarf convection and transit effects as sources of that contamination.
Abstract
Transmission spectroscopy is still the preferred characterization technique for exoplanet atmospheres, although it presents unique challenges which translate into characterization bottlenecks when robust mitigation strategies are missing. Stellar contamination is one of such challenges that can overpower the planetary signal by up to an order of magnitude, and thus not accounting for stellar contamination can lead to significant biases in the derived atmospheric properties. Yet, accounting for stellar contamination may not be straightforward, as important discrepancies exist between state-of-the-art stellar models and measured spectra and between models themselves. Here we explore the extent…
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Atmospheres from very low-mass stars to extrasolar planetsFrance Allard, Derek Homeier · 2012 · Solar and Stellar Astrophysics · cited 105 times · AI summary available
The paper reviews atmosphere modeling across very low-mass stars and extrasolar planets, including unresolved spectroscopic challenges near the M–L transition.
Abstract
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There's more to life than O$_2$: Simulating the detectability of a range of molecules for ground-based high-resolution spectroscopy of transiting terrestrial exoplanetsMiles H. Currie, Victoria S. Meadows, Kaitlin C. Rasmussen · 2023 · Earth and Planetary Astrophysics · cited 10 times · AI summary available
The paper simulates high-resolution transit spectra to assess molecular detectability for terrestrial planets around M dwarfs, rather than modeling convection-driven stellar contamination.
Abstract
Within the next decade, atmospheric O$_2$ on Earth-like M dwarf planets may be accessible with visible--near-infrared, high spectral resolution extremely large ground-based telescope (ELT) instruments. However, the prospects for using ELTs to detect environmental properties that provide context for O$_2$ have not been thoroughly explored. Additional molecules may help indicate planetary habitability, rule out abiotically generated O$_2$, or reveal alternative biosignatures. To understand the accessibility of environmental context using ELT spectra, we simulate high-resolution transit transmission spectra of previously-generated evolved terrestrial atmospheres. We consider inhabited pre-indus…
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EDEN Survey: Small Transiting Planet Detection Limits and Constraints on the Occurrence Rates for Late M Dwarfs within 15 pcJeremy Dietrich, Dániel Apai, Martin Schlecker et al. · 2023 · Earth and Planetary Astrophysics · cited 8 times · AI summary available
The paper monitors nearby late M dwarfs to constrain small transiting-planet occurrence, while the focal paper studies spectra of a transiting planet around an M dwarf.
Abstract
Earth-sized exoplanets that transit nearby, late spectral type red dwarfs will be prime targets for atmospheric characterization in the coming decade. Such systems, however, are difficult to find via wide-field transit surveys like Kepler or TESS. Consequently, the presence of such transiting planets is unexplored and the occurrence rates of short-period Earth-sized planets around late M dwarfs remain poorly constrained. Here, we present the deepest photometric monitoring campaign of 22 nearby late M dwarf stars, using data from over 500 nights on seven 1-2 meter class telescopes. Our survey includes all known single quiescent northern late M dwarfs within 15 pc. We use transit-injection-and…
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Observing M Dwarfs UV and optical flares from a CubeSat and their implications for exoplanets habitabilityJulien Poyatos, Octavi Fors, José Maria Gómez Cama · 2023 · IAC-2022, B4, IP, 33, x70034 · AI summary available
The paper observes M-dwarf flares and considers their consequences for planetary habitability, rather than examining convection’s effects on transit spectroscopy.
Abstract
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