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| Main Authors: | , , , , , , , |
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| Format: | Preprint |
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2025
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| Online Access: | https://arxiv.org/abs/2508.20572 |
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| _version_ | 1866911237400428544 |
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| author | Nail, F. Oklopčić, A. MacLeod, M. Baka, K. Czesla, S. Nagel, E. Linssen, D. Matthijsse, J. |
| author_facet | Nail, F. Oklopčić, A. MacLeod, M. Baka, K. Czesla, S. Nagel, E. Linssen, D. Matthijsse, J. |
| contents | WASP-52 b is an inflated hot Jupiter with a large Roche lobe filling fraction, positioned in the hot Neptune desert. Previous in-transit observations of the helium triplet at 10833 A have reported a range of excess absorption values (1.5%-5.5%) and a lack of net blueshift relative to the planet's rest frame, distinguishing it from other escaping atmospheres. This study investigates the extent and morphology of material escaping from WASP-52 b, assessing whether its outflow resembles a stream-like structure, as suggested for HAT-P-67 b and HAT-P-32 b. We obtained high-resolution spectra with CRIRES+ and CARMENES, covering a broader orbital phase range ($φ\approx \pm0.1, \pm0.2, 0.5$) than previous studies. By analyzing the He I 10833 A line as a tracer of escape, we search for extended absorption beyond transit. Additionally, we explore possible outflow morphologies with three-dimensional (3D) hydrodynamic simulations, coupled with an improved radiative transfer approach, assessing the He I 10833 A triplet. The helium line shows no significant evidence of planetary material at the orbital phases observed in this work, though 3D modeling suggests such a structure could exist below observational detection limits. We conclude that the atmospheric outflow of WASP-52 b can be characterized by an intermediate hydrodynamic escape parameter, placing it in a transitional regime between cold outflows forming a stream-like morphology and hot outflows forming a tail. Additionally, the absence of a detectable in-transit blueshift in the helium line rules out a strong day-to-nightside anisotropy scenario. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2508_20572 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Probing the extent of WASP-52 b's atmosphere. High-resolution observations and 3D modeling insights Nail, F. Oklopčić, A. MacLeod, M. Baka, K. Czesla, S. Nagel, E. Linssen, D. Matthijsse, J. Earth and Planetary Astrophysics WASP-52 b is an inflated hot Jupiter with a large Roche lobe filling fraction, positioned in the hot Neptune desert. Previous in-transit observations of the helium triplet at 10833 A have reported a range of excess absorption values (1.5%-5.5%) and a lack of net blueshift relative to the planet's rest frame, distinguishing it from other escaping atmospheres. This study investigates the extent and morphology of material escaping from WASP-52 b, assessing whether its outflow resembles a stream-like structure, as suggested for HAT-P-67 b and HAT-P-32 b. We obtained high-resolution spectra with CRIRES+ and CARMENES, covering a broader orbital phase range ($φ\approx \pm0.1, \pm0.2, 0.5$) than previous studies. By analyzing the He I 10833 A line as a tracer of escape, we search for extended absorption beyond transit. Additionally, we explore possible outflow morphologies with three-dimensional (3D) hydrodynamic simulations, coupled with an improved radiative transfer approach, assessing the He I 10833 A triplet. The helium line shows no significant evidence of planetary material at the orbital phases observed in this work, though 3D modeling suggests such a structure could exist below observational detection limits. We conclude that the atmospheric outflow of WASP-52 b can be characterized by an intermediate hydrodynamic escape parameter, placing it in a transitional regime between cold outflows forming a stream-like morphology and hot outflows forming a tail. Additionally, the absence of a detectable in-transit blueshift in the helium line rules out a strong day-to-nightside anisotropy scenario. |
| title | Probing the extent of WASP-52 b's atmosphere. High-resolution observations and 3D modeling insights |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2508.20572 |