WASP-69b’s Escaping Envelope Is Confined to a Tail Extending at Least 7 Rp
Studying the escaping atmospheres of highly irradiated exoplanets is critical for understanding the physical mechanisms that shape the demographics of close-in planets. A number of planetary outflows have been observed as excess H/He absorption during/after transit. Such an outflow has been observed...
| Main Authors: | , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad11d0 |
| _version_ | 1797360462276329472 |
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| author | Dakotah Tyler Erik A. Petigura Antonija Oklopčić Trevor J. David |
| author_facet | Dakotah Tyler Erik A. Petigura Antonija Oklopčić Trevor J. David |
| author_sort | Dakotah Tyler |
| collection | DOAJ |
| description | Studying the escaping atmospheres of highly irradiated exoplanets is critical for understanding the physical mechanisms that shape the demographics of close-in planets. A number of planetary outflows have been observed as excess H/He absorption during/after transit. Such an outflow has been observed for WASP-69b by multiple groups that disagree on the geometry and velocity structure of the outflow. Here, we report the detection of this planet’s outflow using Keck/NIRSPEC for the first time. We observed the outflow 1.28 hr after egress until the target set, demonstrating the outflow extends at least 5.8 × 10 ^5 km or 7.5 R _p This detection is significantly longer than previous observations, which report an outflow extending ∼2.2 planet radii just 1 yr prior. The outflow is blueshifted by −23 km s ^−1 in the planetary rest frame. We estimate a current mass-loss rate of 1 M _⊕ Gyr ^−1 . Our observations are most consistent with an outflow that is strongly sculpted by ram pressure from the stellar wind. However, potential variability in the outflow could be due to time-varying interactions with the stellar wind or differences in instrumental precision. |
| first_indexed | 2024-03-08T15:38:53Z |
| format | Article |
| id | doaj.art-8e8da9a414564321bbba8f61e7e7fa1d |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-08T15:38:53Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-8e8da9a414564321bbba8f61e7e7fa1d2024-01-09T15:52:19ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01960212310.3847/1538-4357/ad11d0WASP-69b’s Escaping Envelope Is Confined to a Tail Extending at Least 7 RpDakotah Tyler0https://orcid.org/0000-0003-0298-4667Erik A. Petigura1https://orcid.org/0000-0003-0967-2893Antonija Oklopčić2https://orcid.org/0000-0002-9584-6476Trevor J. David3https://orcid.org/0000-0001-6534-6246Department of Physics and Astronomy, University of California , Los Angeles, CA 90095, USADepartment of Physics and Astronomy, University of California , Los Angeles, CA 90095, USAAnton Pannekoek Institute for Astronomy, University of Amsterdam , Science Park 904, NL-1098 XH Amsterdam, The NetherlandsCenter for Computational Astrophysics, Flatiron Institute , New York, NY 10010, USAStudying the escaping atmospheres of highly irradiated exoplanets is critical for understanding the physical mechanisms that shape the demographics of close-in planets. A number of planetary outflows have been observed as excess H/He absorption during/after transit. Such an outflow has been observed for WASP-69b by multiple groups that disagree on the geometry and velocity structure of the outflow. Here, we report the detection of this planet’s outflow using Keck/NIRSPEC for the first time. We observed the outflow 1.28 hr after egress until the target set, demonstrating the outflow extends at least 5.8 × 10 ^5 km or 7.5 R _p This detection is significantly longer than previous observations, which report an outflow extending ∼2.2 planet radii just 1 yr prior. The outflow is blueshifted by −23 km s ^−1 in the planetary rest frame. We estimate a current mass-loss rate of 1 M _⊕ Gyr ^−1 . Our observations are most consistent with an outflow that is strongly sculpted by ram pressure from the stellar wind. However, potential variability in the outflow could be due to time-varying interactions with the stellar wind or differences in instrumental precision.https://doi.org/10.3847/1538-4357/ad11d0Hot JupitersExoplanet evolutionExoplanet atmospheres |
| spellingShingle | Dakotah Tyler Erik A. Petigura Antonija Oklopčić Trevor J. David WASP-69b’s Escaping Envelope Is Confined to a Tail Extending at Least 7 Rp The Astrophysical Journal Hot Jupiters Exoplanet evolution Exoplanet atmospheres |
| title | WASP-69b’s Escaping Envelope Is Confined to a Tail Extending at Least 7 Rp |
| title_full | WASP-69b’s Escaping Envelope Is Confined to a Tail Extending at Least 7 Rp |
| title_fullStr | WASP-69b’s Escaping Envelope Is Confined to a Tail Extending at Least 7 Rp |
| title_full_unstemmed | WASP-69b’s Escaping Envelope Is Confined to a Tail Extending at Least 7 Rp |
| title_short | WASP-69b’s Escaping Envelope Is Confined to a Tail Extending at Least 7 Rp |
| title_sort | wasp 69b s escaping envelope is confined to a tail extending at least 7 rp |
| topic | Hot Jupiters Exoplanet evolution Exoplanet atmospheres |
| url | https://doi.org/10.3847/1538-4357/ad11d0 |
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