| Title: |
The young HD 73583 (TOI-560) planetary system: two 10-M-circle plus mini-Neptunes transiting a 500-Myr-old, bright, and active K dwarf |
| Authors: |
Barragan, O; Armstrong, DJ; Gandolfi, D; Carleo, I; Vidotto, AA; D'Angelo, CV; Oklopcic, A; Isaacson, H; Oddo, D; Collins, K; Fridlund, M; Sousa, SG; Persson, CM; Hellier, C; Howell, S; Howard, A; Redfield, S; Eisner, N; Georgieva, IY; Dragomir, D; Bayliss, D; Nielsen, LD; Klein, B; Aigrain, S; Zhang, M; Teske, J; Twicken, JD; Jenkins, J; Esposito, M; Van Eylen, V; Rodler, F; Adibekyan, V; Alarcon, J; Anderson, DR; Murphy, JMA; Barrado, D; Barros, SCC; Benneke, B; Bouchy, F; Bryant, EM; Butler, RP; Burt, J; Cabrera, J; Casewell, S; Chaturvedi, P; Cloutier, R; Cochran, WD; Crane, J; Crossfield, I; Crouzet, N |
| Publisher Information: |
Oxford University Press |
| Publication Year: |
2023 |
| Collection: |
Oxford University Research Archive (ORA) |
| Description: |
We present the discovery and characterization of two transiting planets observed by TESS in the light curves of the young and bright (V = 9.67) star HD73583 (TOI-560). We perform an intensive spectroscopic and photometric space-and ground-based follow-up in order to confirm and characterize the system. We found that HD73583 is a young (∼500 Myr) active star with a rotational period of 12.08 ± 0.11 d, and a mass and radius of 0.73 ± 0.02 M and 0.65 ± 0.02 R, respectively. HD 73583 b (Pb = 6.3980420-0.0000062+ 0.0000067 d) has a mass and radius of 10.2-3.1+ 3.4 M and 2.79 ± 0.10 R, respectively, which gives a density of 2.58-0.81+ 0.95 g, cm-3. HD 73583 c (Pc = 18.87974-0.00074+ 0.00086 d) has a mass and radius of 9.7-1.7+ 1.8 M and 2.39-0.09+ 0.10 R, respectively, which translates to a density of 3.88-0.80+ 0.91g, cm-3. Both planets are consistent with worlds made of a solid core surrounded by a volatile envelope. Because of their youth and host star brightness, they both are excellent candidates to perform transmission spectroscopy studies. We expect ongoing atmospheric mass-loss for both planets caused by stellar irradiation. We estimate that the detection of evaporating signatures on H and He would be challenging, but doable with present and future instruments. |
| Document Type: |
article in journal/newspaper |
| Language: |
English |
| Relation: |
https://doi.org/10.1093/mnras/stac638 |
| DOI: |
10.1093/mnras/stac638 |
| Availability: |
https://doi.org/10.1093/mnras/stac638; https://ora.ox.ac.uk/objects/uuid:e9438b98-2a47-4488-af61-832add90b6ad |
| Rights: |
info:eu-repo/semantics/openAccess ; CC Attribution (CC BY) |
| Accession Number: |
edsbas.DE5E2E7C |
| Database: |
BASE |