Giant Planet Occurrence within 0.2 au of Low-luminosity Red Giant Branch Stars with K2

Grunblatt, Samuel K.; Huber, Daniel; Gaidos, Eric; Hon, Marc; Zinn, Joel; Stello, Dennis

doi:10.3847/1538-3881/ab4c35

Cited by 50 publications

(59 citation statements)

References 89 publications

(155 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Dozens of inflated hot Jupiters with radii >1.2 R J have been observed to orbit stars several gigayears old (Guillot & Gautier 2014). Although very young planets (<10 Myr) are expected to have radii this large, it is unclear how such inflated planets can exist around mature main-sequence and even evolved stars (e.g., Grunblatt et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Two Warm, Low-density Sub-Jovian Planets Orbiting Bright Stars in K2 Campaigns 13 and 14

Rodriguez

Eastman

et al. 2018

View full text Add to dashboard Cite

We report the discovery of two planets transiting the bright stars HD 89345 (EPIC 248777106, V=9.376, K=7.721) in K2 Campaign 14 and HD 286123 (EPIC 247098361, V=9.822, K=8.434) in K2 Campaign 13. Both stars are G-type stars, one of which is at or near the end of its main-sequence lifetime, and the other is just over halfway through its main-sequence lifetime. HD 89345 hosts a warm sub-Saturn (0.66R J , 0.11M J , T eq =1100 K) in an 11.81 day orbit. The planet is similar in size to WASP-107b, which falls in the transition region between ice giants and gas giants. HD 286123 hosts a Jupiter-sized, low-mass planet (1.06R J , 0.39 M J , T eq =1000 K) in an 11.17 day, mildly eccentric orbit, with e=0.255±0.035. Given that they orbit relatively evolved main-sequence stars and have orbital periods longer than 10 days, these planets are interesting candidates for studies of gas planet evolution, migration, and (potentially) reinflation. Both planets have spent their entire lifetimes near the proposed stellar irradiation threshold at which giant planets become inflated, and neither shows any sign of radius inflation. They probe the regime where inflation begins to become noticeable and are valuable in constraining planet inflation models. In addition, the brightness of the host stars, combined with large atmospheric scale heights of the planets, makes these two systems favorable targets for transit spectroscopy to study their atmospheres and perhaps provide insight into the physical mechanisms that lead to inflated hot Jupiters.

show abstract

Section: Introductionmentioning

confidence: 99%

Two Warm, Low-density Sub-Jovian Planets Orbiting Bright Stars in K2 Campaigns 13 and 14

Rodriguez

Eastman

et al. 2018

View full text Add to dashboard Cite

show abstract

“…The degeneracy between deposited heating rate and depth can be broken in the case of re-inflated warm Jupiters orbiting post-main-sequence stars. The radii of recently discovered re-inflated warm Jupiters orbiting post-main-sequence stars (Grunblatt et al 2016(Grunblatt et al , 2017(Grunblatt et al , 2019 can be explained with either weak heating at the center of the planet or strong shallow heating. However, post-main-sequence re-inflation occurs much more rapidly for deep heating, and shallow heating cannot explain re-inflation over late stages of main-sequence host stellar evolution.…”

Section: Discussionmentioning

confidence: 99%

“…Future observations of a wide sample of re-inflated warm Jupiters will test mechanisms for radius inflation. TESS will observe ∼ 400, 000 evolved stars, with an expected 0.51±0.29% occurrence rate of close-in re-inflated warm Jupiters around post-main-sequence stars (Grunblatt et al 2019). As a result, we expect that TESS will discover a large sample of of re-inflated warm Jupiters.…”

Section: Using Re-inflation To Test Radius Inflation Mechanismsmentioning

confidence: 93%

“…Including both these constraints, we expect that re-inflated warm Jupiters will be most prevalent around stars with masses 1M M 1.5M . This is the mass range in which current detections of re-inflated warm Jupiters orbiting post-main-sequence stars have been made (Grunblatt et al 2016(Grunblatt et al , 2017(Grunblatt et al , 2019.…”

Section: Post-main-sequence Re-inflationmentioning

confidence: 97%

See 1 more Smart Citation

Reinflation of Warm and Hot Jupiters

Komacek

Thorngren

Lopez

et al. 2020

ApJ

View full text Add to dashboard Cite

Understanding the anomalous radii of many transiting hot gas giant planets is a fundamental problem of planetary science. Recent detections of re-inflated warm Jupiters orbiting post-main-sequence stars and the re-inflation of hot Jupiters while their host stars evolve on the main-sequence may help constrain models for the anomalous radii of hot Jupiters. In this work, we present evolution models studying the re-inflation of gas giants to determine how varying the depth and intensity of deposited heating affects both main-sequence re-inflation of hot Jupiters and post-main-sequence re-inflation of warm Jupiters. We find that deeper heating is required to re-inflate hot Jupiters than is needed to suppress their cooling, and that the timescale of re-inflation decreases with increasing heating rate and depth. We find a strong degeneracy between heating rate and depth, with either strong shallow heating or weak deep heating providing an explanation for main-sequence re-inflation of hot Jupiters. This degeneracy between heating rate and depth can be broken in the case of post-main-sequence re-inflation of warm Jupiters, as the inflation must be rapid to occur within post-main-sequence evolution timescales. We also show that the dependence of heating rate on incident stellar flux inferred from the sample of hot Jupiters can explain re-inflation of both warm and hot Jupiters. TESS will obtain a large sample of warm Jupiters orbiting post-main-sequence stars, which will help to constrain the mechanism(s) causing the anomalous radii of gas giant planets.

show abstract

“…Reichert et al 2019). Grunblatt et al (2019) investigated 2476 low luminosity red giant branch stars observed by the K2 mission (Howell et al 2014). They found a higher occurence rate of planets with size greater than Jupiter in orbital periods less than 10 days compared to around dwarf Sun-like stars.…”

Section: Giant Star Systemsmentioning

confidence: 99%

Asteroid belt survival through stellar evolution: dependence on the stellar mass

Martin

Livio

Smallwood

et al. 2020

Monthly Notices of the Royal Astronomical Society: Letters

View full text Add to dashboard Cite

Polluted white dwarfs are generally accreting terrestrial-like material that may originate from a debris belt like the asteroid belt in the solar system. The fraction of white dwarfs that are polluted drops off significantly for white dwarfs with masses M WD 0.8 M ⊙ . This implies that asteroid belts and planetary systems around main-sequence stars with mass M MS 3 M ⊙ may not form because of the intense radiation from the star. This is in agreement with current debris disc and exoplanet observations. The fraction of white dwarfs that show pollution also drops off significantly for low mass white dwarfs (M WD 0.55 M ⊙ ). However, the low-mass white dwarfs that do show pollution are not currently accreting but have accreted in the past. We suggest that asteroid belts around main sequence stars with masses M MS 2 M ⊙ are not likely to survive the stellar evolution process. The destruction likely occurs during the AGB phase and could be the result of interactions of the asteroids with the stellar wind, the high radiation or, for the lowest mass stars that have an unusually close-in asteroid belt, scattering during the tidal orbital decay of the inner planetary system.

show abstract

Giant Planet Occurrence within 0.2 au of Low-luminosity Red Giant Branch Stars with K2

Cited by 50 publications

References 89 publications

Two Warm, Low-density Sub-Jovian Planets Orbiting Bright Stars in K2 Campaigns 13 and 14

Two Warm, Low-density Sub-Jovian Planets Orbiting Bright Stars in K2 Campaigns 13 and 14

Reinflation of Warm and Hot Jupiters

Asteroid belt survival through stellar evolution: dependence on the stellar mass

Contact Info

Product

Resources

About