TOI-4201: An Early M Dwarf Hosting a Massive Transiting Jupiter Stretching Theories of Core Accretion*

Delamer, Megan; Kanodia, Shubham; Cañas, Caleb I.; Müller, Simon; Helled, Ravit; Lin, Andrea S. J.; Libby-Roberts, Jessica E.; Gupta, Arvind F.; Mahadevan, Suvrath; Teske, Johanna; Butler, R. Paul; Yee, Samuel W.; Crane, Jeffrey D.; Shectman, Stephen; Osip, David; Beletsky, Yuri; Monson, Andrew; Hebb, Leslie; Powers, Luke C.; Wisniewski, John P.; Alvarado-Montes, Jaime A.; Bender, Chad F.; Dong, Jiayin; Han, Te; Ninan, Joe P.; Robertson, Paul; Roy, Arpita; Schwab, Christian; Stefánsson, Guđmundur; Wright, Jason T.

doi:10.3847/2041-8213/ad1a19

Cited by 3 publications

(2 citation statements)

References 130 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The TESS light curves are adopted from Gan et al (2023b), which were extracted through simple aperture photometry. The out-oftransit RVs were from CFHT/SPIRou (Gan et al 2023b), Keck/HIRES (Hartman et al 2023), WIYN/NEID, and Magellan/Planet Finder Spectrograph (PFS) (both from Delamer et al 2024).…”

Section: Discussionmentioning

confidence: 99%

“…Here, we present the first measurement of the RM effect for a hot Jupiter transiting an M dwarf, TOI-4201b. The star is an early M dwarf at a distance about 189 pc, and it hosts a hot Jupiter with an orbital period of 3.58 days (Gan et al 2023b;Hartman et al 2023;Delamer et al 2024). The rest of this Letter is organized as follows: Section 2 details the spectroscopic observations, Section 3 presents the joint-fit analysis, Section 4 discusses the results, and Section 5 describes our conclusions.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The Aligned Orbit of a Hot Jupiter around the M Dwarf TOI-4201

Gan,

Wang,

Dai

et al. 2024

ApJL

Self Cite

View full text Add to dashboard Cite

Measuring the obliquities of stars hosting giant planets may shed light on the dynamical history of planetary systems. Significant efforts have been made to measure the obliquities of FGK stars with hot Jupiters, mainly based on observations of the Rossiter–McLaughlin effect. In contrast, M dwarfs with hot Jupiters have hardly been explored because such systems are rare and often not favorable for such precise observations. Here, we report the first detection of the Rossiter–McLaughlin effect for an M dwarf with a hot Jupiter, TOI-4201, using the Gemini-North/MAROON-X spectrograph. We find TOI-4201 to be well aligned with its giant planet, with a sky-projected obliquity of λ = − 3.0 − 3.2 + 3.7 ° and a true obliquity of ψ = 21.3 − 12.8 + 12.5 ° with an upper limit of 40◦ at a 95% confidence level. The result agrees with dynamically quiet formation or tidal obliquity damping that realigned the system. As the first hot Jupiter around an M dwarf with its obliquity measured, TOI-4201b joins the group of aligned giant planets around cool stars (T eff < 6250 K), as well as the small but growing sample of planets with relatively high planet-to-star mass ratio (M p /M * ≳ 3 × 10−3) that also appear to be mostly aligned.

show abstract

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The Aligned Orbit of a Hot Jupiter around the M Dwarf TOI-4201

Gan,

Wang,

Dai

et al. 2024

ApJL

Self Cite

View full text Add to dashboard Cite

show abstract

Searching for Giant Exoplanets around M-dwarf Stars (GEMS) I: Survey Motivation

Kanodia,

Cañas,

Mahadevan

et al. 2024

Self Cite

View full text Add to dashboard Cite

Recent discoveries of transiting giant exoplanets around M-dwarf stars (GEMS), aided by the all-sky coverage of TESS, are starting to stretch theories of planet formation through the core-accretion scenario. Recent upper limits on their occurrence suggest that they decrease with lower stellar masses, with fewer GEMS around lower-mass stars compared to solar-type. In this paper, we discuss existing GEMS both through confirmed planets, as well as protoplanetary disk observations, and a combination of tests to reconcile these with theoretical predictions. We then introduce the Searching for GEMS survey, where we utilize multidimensional nonparameteric statistics to simulate hypothetical survey scenarios to predict the required sample size of transiting GEMS with mass measurements to robustly compare their bulk-density with canonical hot Jupiters orbiting FGK stars. Our Monte Carlo simulations predict that a robust comparison requires about 40 transiting GEMS (compared to the existing sample of ∼15) with 5σ mass measurements. Furthermore, we discuss the limitations of existing occurrence estimates for GEMS and provide a brief description of our planned systematic search to improve the occurrence rate estimates for GEMS.

show abstract

Can Jupiter’s Atmospheric Metallicity Be Different from the Deep Interior?

Müller,

Helled

2024

ApJ

Self Cite

View full text Add to dashboard Cite

Updated formation and structure models of Jupiter predict a metal-poor envelope. This is at odds with the two to three times solar metallicity measured by the Galileo probe. Additionally, Juno data imply that water and ammonia are enriched. Here, we explore whether Jupiter could have a deep radiative layer separating the atmosphere from the deeper interior. The radiative layer could be caused by a hydrogen-transparency window or depletion of alkali metals. We show that heavy-element accretion during Jupiter’s evolution could lead to the desired atmospheric enrichment and that this configuration would be stable over billions of years. The origin of the heavy elements could be cumulative small impacts or one large impact. The preferred scenario requires a deep radiative zone, due to a local reduction of the opacity at ∼2000 K by ∼90%, which is supported by Juno data, and vertical mixing through the boundary with an efficiency similar to that of molecular diffusion (D ≲ 10−2 cm2 s−1). Therefore, most of Jupiter’s molecular envelope could have solar composition while its uppermost atmosphere is enriched with heavier elements. The enrichment likely originates from the accretion of solid objects. This possibility resolves the long-standing mismatch between Jupiter’s interior models and atmospheric composition measurements. Furthermore, our results imply that the measured atmospheric composition of exoplanets does not necessarily reflect their bulk compositions. We also investigate whether the enrichment could be due to the erosion of a dilute core and show that this is highly unlikely. The core-erosion scenario is inconsistent with evolution calculations, the deep radiative layer, and published interior models.

show abstract

TOI-4201: An Early M Dwarf Hosting a Massive Transiting Jupiter Stretching Theories of Core Accretion*

Cited by 3 publications

References 130 publications

The Aligned Orbit of a Hot Jupiter around the M Dwarf TOI-4201

The Aligned Orbit of a Hot Jupiter around the M Dwarf TOI-4201

Searching for Giant Exoplanets around M-dwarf Stars (GEMS) I: Survey Motivation

Can Jupiter’s Atmospheric Metallicity Be Different from the Deep Interior?

Contact Info

Product

Resources

About