A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation

Atmospheric escape shapes the fate of exoplanets, with statistical evidence for transformative mass loss imprinted across the mass–radius–insolation distribution. Here, we present transit spectroscopy of the highly irradiated, low-gravity, inflated hot Saturn HAT-P-67 b. The Habitable Zone Planet Fi...
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Autor*in:	Michael Gully-Santiago [verfasserIn] Caroline V. Morley [verfasserIn] Jessica Luna [verfasserIn] Morgan MacLeod [verfasserIn] Antonija Oklopčić [verfasserIn] Aishwarya Ganesh [verfasserIn] Quang H. Tran [verfasserIn] Zhoujian Zhang [verfasserIn] Brendan P. Bowler [verfasserIn] William D. Cochran [verfasserIn] Daniel M. Krolikowski [verfasserIn] Suvrath Mahadevan [verfasserIn] Joe P. Ninan [verfasserIn] Guđmundur Stefánsson [verfasserIn] Andrew Vanderburg [verfasserIn] Joseph A. Zalesky [verfasserIn] Gregory R. Zeimann [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2024

Schlagwörter:	Exoplanet atmospheres Exoplanet evolution Exoplanet atmospheric dynamics Exoplanet atmospheric variability Stellar winds High resolution spectroscopy

Übergeordnetes Werk:	In: The Astronomical Journal - IOP Publishing, 2022, 167(2024), 4, p 142
Übergeordnetes Werk:	volume:167 ; year:2024 ; number:4, p 142

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/1538-3881/ad1ee8

Katalog-ID:	DOAJ101447485

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allfields	10.3847/1538-3881/ad1ee8 doi (DE-627)DOAJ101447485 (DE-599)DOAJ33715524ec2e4c0f98d1512d3433a26b DE-627 ger DE-627 rakwb eng QB1-991 Michael Gully-Santiago verfasserin aut A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Atmospheric escape shapes the fate of exoplanets, with statistical evidence for transformative mass loss imprinted across the mass–radius–insolation distribution. Here, we present transit spectroscopy of the highly irradiated, low-gravity, inflated hot Saturn HAT-P-67 b. The Habitable Zone Planet Finder spectra show a detection of up to 10% absorption depth of the 10833 Å helium triplet. The 13.8 hr of on-sky integration time over 39 nights sample the entire planet orbit, uncovering excess helium absorption preceding the transit by up to 130 planetary radii in a large leading tail. This configuration can be understood as the escaping material overflowing its small Roche lobe and advecting most of the gas into the stellar—and not planetary—rest frame, consistent with the Doppler velocity structure seen in the helium line profiles. The prominent leading tail serves as direct evidence for dayside mass loss with a strong day-/nightside asymmetry. We see some transit-to-transit variability in the line profile, consistent with the interplay of stellar and planetary winds. We employ one-dimensional Parker wind models to estimate the mass-loss rate, finding values on the order of 2 × 10 ^13 g s ^−1 , with large uncertainties owing to the unknown X-ray and ultraviolet (XUV) flux of the F host star. The large mass loss in HAT-P-67 b represents a valuable example of an inflated hot Saturn, a class of planets recently identified to be rare, as their atmospheres are predicted to evaporate quickly. We contrast two physical mechanisms for runaway evaporation: ohmic dissipation and XUV irradiation, slightly favoring the latter. Exoplanet atmospheres Exoplanet evolution Exoplanet atmospheric dynamics Exoplanet atmospheric variability Stellar winds High resolution spectroscopy Astronomy Caroline V. Morley verfasserin aut Jessica Luna verfasserin aut Morgan MacLeod verfasserin aut Antonija Oklopčić verfasserin aut Aishwarya Ganesh verfasserin aut Quang H. Tran verfasserin aut Zhoujian Zhang verfasserin aut Brendan P. Bowler verfasserin aut William D. Cochran verfasserin aut Daniel M. Krolikowski verfasserin aut Suvrath Mahadevan verfasserin aut Joe P. Ninan verfasserin aut Guđmundur Stefánsson verfasserin aut Andrew Vanderburg verfasserin aut Joseph A. Zalesky verfasserin aut Gregory R. Zeimann verfasserin aut In The Astronomical Journal IOP Publishing, 2022 167(2024), 4, p 142 (DE-627)312175647 (DE-600)2003104-X 15383881 nnns volume:167 year:2024 number:4, p 142 https://doi.org/10.3847/1538-3881/ad1ee8 kostenfrei https://doaj.org/article/33715524ec2e4c0f98d1512d3433a26b kostenfrei https://doi.org/10.3847/1538-3881/ad1ee8 kostenfrei https://doaj.org/toc/1538-3881 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2110 GBV_ILN_2129 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 167 2024 4, p 142
spelling	10.3847/1538-3881/ad1ee8 doi (DE-627)DOAJ101447485 (DE-599)DOAJ33715524ec2e4c0f98d1512d3433a26b DE-627 ger DE-627 rakwb eng QB1-991 Michael Gully-Santiago verfasserin aut A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Atmospheric escape shapes the fate of exoplanets, with statistical evidence for transformative mass loss imprinted across the mass–radius–insolation distribution. Here, we present transit spectroscopy of the highly irradiated, low-gravity, inflated hot Saturn HAT-P-67 b. The Habitable Zone Planet Finder spectra show a detection of up to 10% absorption depth of the 10833 Å helium triplet. The 13.8 hr of on-sky integration time over 39 nights sample the entire planet orbit, uncovering excess helium absorption preceding the transit by up to 130 planetary radii in a large leading tail. This configuration can be understood as the escaping material overflowing its small Roche lobe and advecting most of the gas into the stellar—and not planetary—rest frame, consistent with the Doppler velocity structure seen in the helium line profiles. The prominent leading tail serves as direct evidence for dayside mass loss with a strong day-/nightside asymmetry. We see some transit-to-transit variability in the line profile, consistent with the interplay of stellar and planetary winds. We employ one-dimensional Parker wind models to estimate the mass-loss rate, finding values on the order of 2 × 10 ^13 g s ^−1 , with large uncertainties owing to the unknown X-ray and ultraviolet (XUV) flux of the F host star. The large mass loss in HAT-P-67 b represents a valuable example of an inflated hot Saturn, a class of planets recently identified to be rare, as their atmospheres are predicted to evaporate quickly. We contrast two physical mechanisms for runaway evaporation: ohmic dissipation and XUV irradiation, slightly favoring the latter. Exoplanet atmospheres Exoplanet evolution Exoplanet atmospheric dynamics Exoplanet atmospheric variability Stellar winds High resolution spectroscopy Astronomy Caroline V. Morley verfasserin aut Jessica Luna verfasserin aut Morgan MacLeod verfasserin aut Antonija Oklopčić verfasserin aut Aishwarya Ganesh verfasserin aut Quang H. Tran verfasserin aut Zhoujian Zhang verfasserin aut Brendan P. Bowler verfasserin aut William D. Cochran verfasserin aut Daniel M. Krolikowski verfasserin aut Suvrath Mahadevan verfasserin aut Joe P. Ninan verfasserin aut Guđmundur Stefánsson verfasserin aut Andrew Vanderburg verfasserin aut Joseph A. Zalesky verfasserin aut Gregory R. Zeimann verfasserin aut In The Astronomical Journal IOP Publishing, 2022 167(2024), 4, p 142 (DE-627)312175647 (DE-600)2003104-X 15383881 nnns volume:167 year:2024 number:4, p 142 https://doi.org/10.3847/1538-3881/ad1ee8 kostenfrei https://doaj.org/article/33715524ec2e4c0f98d1512d3433a26b kostenfrei https://doi.org/10.3847/1538-3881/ad1ee8 kostenfrei https://doaj.org/toc/1538-3881 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2110 GBV_ILN_2129 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 167 2024 4, p 142
allfields_unstemmed	10.3847/1538-3881/ad1ee8 doi (DE-627)DOAJ101447485 (DE-599)DOAJ33715524ec2e4c0f98d1512d3433a26b DE-627 ger DE-627 rakwb eng QB1-991 Michael Gully-Santiago verfasserin aut A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Atmospheric escape shapes the fate of exoplanets, with statistical evidence for transformative mass loss imprinted across the mass–radius–insolation distribution. Here, we present transit spectroscopy of the highly irradiated, low-gravity, inflated hot Saturn HAT-P-67 b. The Habitable Zone Planet Finder spectra show a detection of up to 10% absorption depth of the 10833 Å helium triplet. The 13.8 hr of on-sky integration time over 39 nights sample the entire planet orbit, uncovering excess helium absorption preceding the transit by up to 130 planetary radii in a large leading tail. This configuration can be understood as the escaping material overflowing its small Roche lobe and advecting most of the gas into the stellar—and not planetary—rest frame, consistent with the Doppler velocity structure seen in the helium line profiles. The prominent leading tail serves as direct evidence for dayside mass loss with a strong day-/nightside asymmetry. We see some transit-to-transit variability in the line profile, consistent with the interplay of stellar and planetary winds. We employ one-dimensional Parker wind models to estimate the mass-loss rate, finding values on the order of 2 × 10 ^13 g s ^−1 , with large uncertainties owing to the unknown X-ray and ultraviolet (XUV) flux of the F host star. The large mass loss in HAT-P-67 b represents a valuable example of an inflated hot Saturn, a class of planets recently identified to be rare, as their atmospheres are predicted to evaporate quickly. We contrast two physical mechanisms for runaway evaporation: ohmic dissipation and XUV irradiation, slightly favoring the latter. Exoplanet atmospheres Exoplanet evolution Exoplanet atmospheric dynamics Exoplanet atmospheric variability Stellar winds High resolution spectroscopy Astronomy Caroline V. Morley verfasserin aut Jessica Luna verfasserin aut Morgan MacLeod verfasserin aut Antonija Oklopčić verfasserin aut Aishwarya Ganesh verfasserin aut Quang H. Tran verfasserin aut Zhoujian Zhang verfasserin aut Brendan P. Bowler verfasserin aut William D. Cochran verfasserin aut Daniel M. Krolikowski verfasserin aut Suvrath Mahadevan verfasserin aut Joe P. Ninan verfasserin aut Guđmundur Stefánsson verfasserin aut Andrew Vanderburg verfasserin aut Joseph A. Zalesky verfasserin aut Gregory R. Zeimann verfasserin aut In The Astronomical Journal IOP Publishing, 2022 167(2024), 4, p 142 (DE-627)312175647 (DE-600)2003104-X 15383881 nnns volume:167 year:2024 number:4, p 142 https://doi.org/10.3847/1538-3881/ad1ee8 kostenfrei https://doaj.org/article/33715524ec2e4c0f98d1512d3433a26b kostenfrei https://doi.org/10.3847/1538-3881/ad1ee8 kostenfrei https://doaj.org/toc/1538-3881 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2110 GBV_ILN_2129 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 167 2024 4, p 142
allfieldsGer	10.3847/1538-3881/ad1ee8 doi (DE-627)DOAJ101447485 (DE-599)DOAJ33715524ec2e4c0f98d1512d3433a26b DE-627 ger DE-627 rakwb eng QB1-991 Michael Gully-Santiago verfasserin aut A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Atmospheric escape shapes the fate of exoplanets, with statistical evidence for transformative mass loss imprinted across the mass–radius–insolation distribution. Here, we present transit spectroscopy of the highly irradiated, low-gravity, inflated hot Saturn HAT-P-67 b. The Habitable Zone Planet Finder spectra show a detection of up to 10% absorption depth of the 10833 Å helium triplet. The 13.8 hr of on-sky integration time over 39 nights sample the entire planet orbit, uncovering excess helium absorption preceding the transit by up to 130 planetary radii in a large leading tail. This configuration can be understood as the escaping material overflowing its small Roche lobe and advecting most of the gas into the stellar—and not planetary—rest frame, consistent with the Doppler velocity structure seen in the helium line profiles. The prominent leading tail serves as direct evidence for dayside mass loss with a strong day-/nightside asymmetry. We see some transit-to-transit variability in the line profile, consistent with the interplay of stellar and planetary winds. We employ one-dimensional Parker wind models to estimate the mass-loss rate, finding values on the order of 2 × 10 ^13 g s ^−1 , with large uncertainties owing to the unknown X-ray and ultraviolet (XUV) flux of the F host star. The large mass loss in HAT-P-67 b represents a valuable example of an inflated hot Saturn, a class of planets recently identified to be rare, as their atmospheres are predicted to evaporate quickly. We contrast two physical mechanisms for runaway evaporation: ohmic dissipation and XUV irradiation, slightly favoring the latter. Exoplanet atmospheres Exoplanet evolution Exoplanet atmospheric dynamics Exoplanet atmospheric variability Stellar winds High resolution spectroscopy Astronomy Caroline V. Morley verfasserin aut Jessica Luna verfasserin aut Morgan MacLeod verfasserin aut Antonija Oklopčić verfasserin aut Aishwarya Ganesh verfasserin aut Quang H. Tran verfasserin aut Zhoujian Zhang verfasserin aut Brendan P. Bowler verfasserin aut William D. Cochran verfasserin aut Daniel M. Krolikowski verfasserin aut Suvrath Mahadevan verfasserin aut Joe P. Ninan verfasserin aut Guđmundur Stefánsson verfasserin aut Andrew Vanderburg verfasserin aut Joseph A. Zalesky verfasserin aut Gregory R. Zeimann verfasserin aut In The Astronomical Journal IOP Publishing, 2022 167(2024), 4, p 142 (DE-627)312175647 (DE-600)2003104-X 15383881 nnns volume:167 year:2024 number:4, p 142 https://doi.org/10.3847/1538-3881/ad1ee8 kostenfrei https://doaj.org/article/33715524ec2e4c0f98d1512d3433a26b kostenfrei https://doi.org/10.3847/1538-3881/ad1ee8 kostenfrei https://doaj.org/toc/1538-3881 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2110 GBV_ILN_2129 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 167 2024 4, p 142
allfieldsSound	10.3847/1538-3881/ad1ee8 doi (DE-627)DOAJ101447485 (DE-599)DOAJ33715524ec2e4c0f98d1512d3433a26b DE-627 ger DE-627 rakwb eng QB1-991 Michael Gully-Santiago verfasserin aut A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Atmospheric escape shapes the fate of exoplanets, with statistical evidence for transformative mass loss imprinted across the mass–radius–insolation distribution. Here, we present transit spectroscopy of the highly irradiated, low-gravity, inflated hot Saturn HAT-P-67 b. The Habitable Zone Planet Finder spectra show a detection of up to 10% absorption depth of the 10833 Å helium triplet. The 13.8 hr of on-sky integration time over 39 nights sample the entire planet orbit, uncovering excess helium absorption preceding the transit by up to 130 planetary radii in a large leading tail. This configuration can be understood as the escaping material overflowing its small Roche lobe and advecting most of the gas into the stellar—and not planetary—rest frame, consistent with the Doppler velocity structure seen in the helium line profiles. The prominent leading tail serves as direct evidence for dayside mass loss with a strong day-/nightside asymmetry. We see some transit-to-transit variability in the line profile, consistent with the interplay of stellar and planetary winds. We employ one-dimensional Parker wind models to estimate the mass-loss rate, finding values on the order of 2 × 10 ^13 g s ^−1 , with large uncertainties owing to the unknown X-ray and ultraviolet (XUV) flux of the F host star. The large mass loss in HAT-P-67 b represents a valuable example of an inflated hot Saturn, a class of planets recently identified to be rare, as their atmospheres are predicted to evaporate quickly. We contrast two physical mechanisms for runaway evaporation: ohmic dissipation and XUV irradiation, slightly favoring the latter. Exoplanet atmospheres Exoplanet evolution Exoplanet atmospheric dynamics Exoplanet atmospheric variability Stellar winds High resolution spectroscopy Astronomy Caroline V. Morley verfasserin aut Jessica Luna verfasserin aut Morgan MacLeod verfasserin aut Antonija Oklopčić verfasserin aut Aishwarya Ganesh verfasserin aut Quang H. Tran verfasserin aut Zhoujian Zhang verfasserin aut Brendan P. Bowler verfasserin aut William D. Cochran verfasserin aut Daniel M. Krolikowski verfasserin aut Suvrath Mahadevan verfasserin aut Joe P. Ninan verfasserin aut Guđmundur Stefánsson verfasserin aut Andrew Vanderburg verfasserin aut Joseph A. Zalesky verfasserin aut Gregory R. Zeimann verfasserin aut In The Astronomical Journal IOP Publishing, 2022 167(2024), 4, p 142 (DE-627)312175647 (DE-600)2003104-X 15383881 nnns volume:167 year:2024 number:4, p 142 https://doi.org/10.3847/1538-3881/ad1ee8 kostenfrei https://doaj.org/article/33715524ec2e4c0f98d1512d3433a26b kostenfrei https://doi.org/10.3847/1538-3881/ad1ee8 kostenfrei https://doaj.org/toc/1538-3881 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2110 GBV_ILN_2129 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 167 2024 4, p 142
language	English
source	In The Astronomical Journal 167(2024), 4, p 142 volume:167 year:2024 number:4, p 142
sourceStr	In The Astronomical Journal 167(2024), 4, p 142 volume:167 year:2024 number:4, p 142
format_phy_str_mv	Article
institution	findex.gbv.de
topic_facet	Exoplanet atmospheres Exoplanet evolution Exoplanet atmospheric dynamics Exoplanet atmospheric variability Stellar winds High resolution spectroscopy Astronomy
isfreeaccess_bool	true
container_title	The Astronomical Journal
authorswithroles_txt_mv	Michael Gully-Santiago @@aut@@ Caroline V. Morley @@aut@@ Jessica Luna @@aut@@ Morgan MacLeod @@aut@@ Antonija Oklopčić @@aut@@ Aishwarya Ganesh @@aut@@ Quang H. Tran @@aut@@ Zhoujian Zhang @@aut@@ Brendan P. Bowler @@aut@@ William D. Cochran @@aut@@ Daniel M. Krolikowski @@aut@@ Suvrath Mahadevan @@aut@@ Joe P. Ninan @@aut@@ Guđmundur Stefánsson @@aut@@ Andrew Vanderburg @@aut@@ Joseph A. Zalesky @@aut@@ Gregory R. Zeimann @@aut@@
publishDateDaySort_date	2024-01-01T00:00:00Z
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language_de	englisch
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callnumber-first	Q - Science
author	Michael Gully-Santiago
spellingShingle	Michael Gully-Santiago misc QB1-991 misc Exoplanet atmospheres misc Exoplanet evolution misc Exoplanet atmospheric dynamics misc Exoplanet atmospheric variability misc Stellar winds misc High resolution spectroscopy misc Astronomy A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
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topic_title	QB1-991 A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation Exoplanet atmospheres Exoplanet evolution Exoplanet atmospheric dynamics Exoplanet atmospheric variability Stellar winds High resolution spectroscopy
topic	misc QB1-991 misc Exoplanet atmospheres misc Exoplanet evolution misc Exoplanet atmospheric dynamics misc Exoplanet atmospheric variability misc Stellar winds misc High resolution spectroscopy misc Astronomy
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title	A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
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title_full	A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
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author_browse	Michael Gully-Santiago Caroline V. Morley Jessica Luna Morgan MacLeod Antonija Oklopčić Aishwarya Ganesh Quang H. Tran Zhoujian Zhang Brendan P. Bowler William D. Cochran Daniel M. Krolikowski Suvrath Mahadevan Joe P. Ninan Guđmundur Stefánsson Andrew Vanderburg Joseph A. Zalesky Gregory R. Zeimann
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title_sort	large and variable leading tail of helium in a hot saturn undergoing runaway inflation
callnumber	QB1-991
title_auth	A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
abstract	Atmospheric escape shapes the fate of exoplanets, with statistical evidence for transformative mass loss imprinted across the mass–radius–insolation distribution. Here, we present transit spectroscopy of the highly irradiated, low-gravity, inflated hot Saturn HAT-P-67 b. The Habitable Zone Planet Finder spectra show a detection of up to 10% absorption depth of the 10833 Å helium triplet. The 13.8 hr of on-sky integration time over 39 nights sample the entire planet orbit, uncovering excess helium absorption preceding the transit by up to 130 planetary radii in a large leading tail. This configuration can be understood as the escaping material overflowing its small Roche lobe and advecting most of the gas into the stellar—and not planetary—rest frame, consistent with the Doppler velocity structure seen in the helium line profiles. The prominent leading tail serves as direct evidence for dayside mass loss with a strong day-/nightside asymmetry. We see some transit-to-transit variability in the line profile, consistent with the interplay of stellar and planetary winds. We employ one-dimensional Parker wind models to estimate the mass-loss rate, finding values on the order of 2 × 10 ^13 g s ^−1 , with large uncertainties owing to the unknown X-ray and ultraviolet (XUV) flux of the F host star. The large mass loss in HAT-P-67 b represents a valuable example of an inflated hot Saturn, a class of planets recently identified to be rare, as their atmospheres are predicted to evaporate quickly. We contrast two physical mechanisms for runaway evaporation: ohmic dissipation and XUV irradiation, slightly favoring the latter.
abstractGer	Atmospheric escape shapes the fate of exoplanets, with statistical evidence for transformative mass loss imprinted across the mass–radius–insolation distribution. Here, we present transit spectroscopy of the highly irradiated, low-gravity, inflated hot Saturn HAT-P-67 b. The Habitable Zone Planet Finder spectra show a detection of up to 10% absorption depth of the 10833 Å helium triplet. The 13.8 hr of on-sky integration time over 39 nights sample the entire planet orbit, uncovering excess helium absorption preceding the transit by up to 130 planetary radii in a large leading tail. This configuration can be understood as the escaping material overflowing its small Roche lobe and advecting most of the gas into the stellar—and not planetary—rest frame, consistent with the Doppler velocity structure seen in the helium line profiles. The prominent leading tail serves as direct evidence for dayside mass loss with a strong day-/nightside asymmetry. We see some transit-to-transit variability in the line profile, consistent with the interplay of stellar and planetary winds. We employ one-dimensional Parker wind models to estimate the mass-loss rate, finding values on the order of 2 × 10 ^13 g s ^−1 , with large uncertainties owing to the unknown X-ray and ultraviolet (XUV) flux of the F host star. The large mass loss in HAT-P-67 b represents a valuable example of an inflated hot Saturn, a class of planets recently identified to be rare, as their atmospheres are predicted to evaporate quickly. We contrast two physical mechanisms for runaway evaporation: ohmic dissipation and XUV irradiation, slightly favoring the latter.
abstract_unstemmed	Atmospheric escape shapes the fate of exoplanets, with statistical evidence for transformative mass loss imprinted across the mass–radius–insolation distribution. Here, we present transit spectroscopy of the highly irradiated, low-gravity, inflated hot Saturn HAT-P-67 b. The Habitable Zone Planet Finder spectra show a detection of up to 10% absorption depth of the 10833 Å helium triplet. The 13.8 hr of on-sky integration time over 39 nights sample the entire planet orbit, uncovering excess helium absorption preceding the transit by up to 130 planetary radii in a large leading tail. This configuration can be understood as the escaping material overflowing its small Roche lobe and advecting most of the gas into the stellar—and not planetary—rest frame, consistent with the Doppler velocity structure seen in the helium line profiles. The prominent leading tail serves as direct evidence for dayside mass loss with a strong day-/nightside asymmetry. We see some transit-to-transit variability in the line profile, consistent with the interplay of stellar and planetary winds. We employ one-dimensional Parker wind models to estimate the mass-loss rate, finding values on the order of 2 × 10 ^13 g s ^−1 , with large uncertainties owing to the unknown X-ray and ultraviolet (XUV) flux of the F host star. The large mass loss in HAT-P-67 b represents a valuable example of an inflated hot Saturn, a class of planets recently identified to be rare, as their atmospheres are predicted to evaporate quickly. We contrast two physical mechanisms for runaway evaporation: ohmic dissipation and XUV irradiation, slightly favoring the latter.
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container_issue	4, p 142
title_short	A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation
url	https://doi.org/10.3847/1538-3881/ad1ee8 https://doaj.org/article/33715524ec2e4c0f98d1512d3433a26b https://doaj.org/toc/1538-3881
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