HIP 41378 observed by CHEOPS: Where is planet d?
(2024) In Astronomy and Astrophysics 686.- Abstract
- HIP 41378 d is a long-period planet that has only been observed to transit twice, three years apart, with K2. According to stability considerations and a partial detection of the Rossiter- McLaughlin effect, Pd = 278.36 d has been determined to be the most likely orbital period. We targeted HIP 41378 d with CHEOPS at the predicted transit timing based on Pd = 278.36 d, but the observations show no transit. We find that large (> 22.4 h) transit timing variations (TTVs) could explain this non-detection during the CHEOPS observation window. We also investigated the possibility of an incorrect orbital solution, which would have major implications for our knowledge of this system. If Pd ≠ 278.36 d, the periods that minimize the eccentricity... (More)
- HIP 41378 d is a long-period planet that has only been observed to transit twice, three years apart, with K2. According to stability considerations and a partial detection of the Rossiter- McLaughlin effect, Pd = 278.36 d has been determined to be the most likely orbital period. We targeted HIP 41378 d with CHEOPS at the predicted transit timing based on Pd = 278.36 d, but the observations show no transit. We find that large (> 22.4 h) transit timing variations (TTVs) could explain this non-detection during the CHEOPS observation window. We also investigated the possibility of an incorrect orbital solution, which would have major implications for our knowledge of this system. If Pd ≠ 278.36 d, the periods that minimize the eccentricity would be 101.22 d and 371.14 d. The shortest orbital period will be tested by TESS, which will observe HIP 41378 in Sector 88 starting in January 2025. Our study shows the importance of a mission like CHEOPS, which today is the only mission able to make long observations (i.e., from space) to track the ephemeris of long-period planets possibly affected by large TTVs. © 2024 The Authors. (Less)
Please use this url to cite or link to this publication:
https://lup.lub.lu.se/record/e033c414-bc5a-40ac-89cb-ac3faad2e4d9
- author
- Sulis, S. ; Davies, M.B. LU ; Korth, J. LU and Zingales, T.
- author collaboration
- organization
- publishing date
- 2024
- type
- Contribution to journal
- publication status
- published
- subject
- keywords
- HIP 41378, individual, Planets and satellites, Orbits, Satellites, Individual, Most likely, Non-detection, Observation window, Orbital periods, Orbitals, Timing variations, Transit timing, Planets
- in
- Astronomy and Astrophysics
- volume
- 686
- article number
- L18
- publisher
- EDP Sciences
- external identifiers
-
- scopus:85201083317
- ISSN
- 0004-6361
- DOI
- 10.1051/0004-6361/202449689
- language
- English
- LU publication?
- yes
- id
- e033c414-bc5a-40ac-89cb-ac3faad2e4d9
- date added to LUP
- 2024-10-02 13:09:39
- date last changed
- 2024-10-02 13:09:39
@article{e033c414-bc5a-40ac-89cb-ac3faad2e4d9, abstract = {{HIP 41378 d is a long-period planet that has only been observed to transit twice, three years apart, with K2. According to stability considerations and a partial detection of the Rossiter- McLaughlin effect, Pd = 278.36 d has been determined to be the most likely orbital period. We targeted HIP 41378 d with CHEOPS at the predicted transit timing based on Pd = 278.36 d, but the observations show no transit. We find that large (> 22.4 h) transit timing variations (TTVs) could explain this non-detection during the CHEOPS observation window. We also investigated the possibility of an incorrect orbital solution, which would have major implications for our knowledge of this system. If Pd ≠ 278.36 d, the periods that minimize the eccentricity would be 101.22 d and 371.14 d. The shortest orbital period will be tested by TESS, which will observe HIP 41378 in Sector 88 starting in January 2025. Our study shows the importance of a mission like CHEOPS, which today is the only mission able to make long observations (i.e., from space) to track the ephemeris of long-period planets possibly affected by large TTVs. © 2024 The Authors.}}, author = {{Sulis, S. and Davies, M.B. and Korth, J. and Zingales, T.}}, issn = {{0004-6361}}, keywords = {{HIP 41378; individual; Planets and satellites; Orbits; Satellites; Individual; Most likely; Non-detection; Observation window; Orbital periods; Orbitals; Timing variations; Transit timing; Planets}}, language = {{eng}}, publisher = {{EDP Sciences}}, series = {{Astronomy and Astrophysics}}, title = {{HIP 41378 observed by CHEOPS: Where is planet d?}}, url = {{http://dx.doi.org/10.1051/0004-6361/202449689}}, doi = {{10.1051/0004-6361/202449689}}, volume = {{686}}, year = {{2024}}, }