J/A+A/679/L12 Close-in planets around fast-rotating stars (Garcia+, 2023)
Stellar spectral-type (mass) dependence of the dearth of close-in planets around
fast-rotating stars. Architecture of Kepler confirmed single exoplanet systems
compared to star-planet evolution models.
Garcia R.A., Gourves C., Santos A.R.G., Strugarek A., Godoy-Rivera D.,
Mathur S., Delsanti V., Breton S. N., Beck P. G., Brun A. S., Mathis S.
<Astron. Astrophys. 679, L12 (2023)>
=2023A&A...679L..12G 2023A&A...679L..12G (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Stars, diameters ;
Effective temperatures ; Abundances, [Fe/H] ; Optical
Keywords: planet-star interactions - stars: evolution - stars: rotation -
stars: low-mass - stars: activity - techniques: photometric -
Abstract:
In 2013 a dearth of close-in planets around fast-rotating host stars
was found using statistical tests on Kepler data. The addition of more
Kepler and Transiting Exoplanet Survey Satellite (TESS) systems in
2022 filled this region of the diagram of stellar rotation period
(Prot) versus the planet orbital period (Porb). We revisited the Prot
extraction of Kepler planet-host stars, we classify the stars by their
spectral type, and we studied their Prot-Porb relations. We only
used confirmed exoplanet systems to minimize biases. In order to learn
about the physical processes at work, we used the star-planet
evolution code ESPEM (French acronym for Evolution of Planetary
Systems and Magnetism) to compute a realistic population synthesis of
exoplanet systems and compared them with observations. Because ESPEM
works with a single planet orbiting around a single main-sequence
star, we limit our study to this population of Kepler observed systems
filtering out binaries, evolved stars, and multi-planets. We find in
both, observations and simulations, the existence of a dearth in
close-in planets orbiting around fast-rotating stars, with a
dependence on the stellar spectral type (F, G, and K), which is a
proxy of the mass in our sample of stars. There is a change in the
edge of the dearth as a function of the spectral type (and mass). It
moves towards shorter Prot as temperature (and mass) increases, making
the dearth look smaller. Realistic formation hypotheses included in
the model and the proper treatment of tidal and magnetic migration are
enough to qualitatively explain the dearth of hot planets around
fast-rotating stars and the uncovered trend with spectral type.
Description:
The values of Prot were obtained using the automatic selection
procedure described in Santos et al. (2021ApJS..255...17S 2021ApJS..255...17S, Cat.
J/ApJS/255/17) coupled to the machine learning algorithm ROOSTER
(Breton et al., 2021A&A...647A.125B 2021A&A...647A.125B). Moreover, all the stars (with
and without a retrieved Prot) were visually inspected using the three
new folded-KEPSEIMIC and the PDC-MAP LCs. In Table 1 we provide the
list of 796 stars with Prot after the visual checks.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 129 796 Stellar and exoplanet properties
--------------------------------------------------------------------------------
See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 I8 --- KIC Kepler Input Catalog ID
10- 21 A12 --- HostID Kepler Host ID (Kepler-NNNN)
23- 30 F8.3 d Porb Planetary orbital period
32- 36 F5.3 d E_Porb Upper uncertainty on Porb
38- 42 F5.3 d e_Porb Lower uncertainty on Porb
44- 48 F5.2 Rgeo Rp Planetary radius
50- 53 F4.2 Rgeo E_Rp Upper uncertainty on Rp
55- 58 F4.2 Rgeo e_Rp Lower uncertainty on Rp
60- 64 F5.2 d Prot Rotation period
66- 69 F4.2 d E_Prot Uncertainty on Prot
71- 74 I4 K Teff Effective temperature
76- 78 I3 K E_Teff Upper uncertainty on Teff
80- 82 I3 K e_Teff Lower uncertainty on Teff
84- 88 F5.3 [cm-2] logg Log surface gravity
90- 94 F5.3 [cm-2] E_logg Upper uncertainty on logg
96-100 F5.3 [cm-2] e_logg Lower uncertainty on logg
102-107 F6.3 --- [Fe/H] Metallicity
109-113 F5.3 --- E_[Fe/H] Upper uncertainty on [Fe/H]
115-119 F5.3 --- e_[Fe/H] Lower uncertainty on [Fe/H]
121-124 I4 --- Flag1 [1/3]?=-999 Type of rotation signal (1)
126-129 I4 --- Flag2 [1/2]?=-999 Flag binary/evolved (2)
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Note (1): Type of rotation signal as follows:
1 = close-in binary candidate
2 = true Prot could be x2
3 = hump & spike candidates
Note (2): Flag binary/evolved as follows:
1 = binary or evolved star
2 = Gaia colors missing
--------------------------------------------------------------------------------
History:
From Rafael Garcia, rgarcia(at)cea.fr
Acknowledgements:
The authors of this paper acknowledge James Davenport for providing
the KIC2TIC as an open source code at github. We also thank David V.
Martin for providing an updated list of known circumbinary exoplanet
hosts and C. Le Poncin-Lafitte for his contribution to ESPEM. A.S.B,
S.N.B., R.A.G., A.S., and St.M. acknowledge the support from the PLATO
Centre National D'Etudes Spatiales grant. A.S. acknowledges
funding from the European Union's Horizon-2020 research and
innovation program (grant agreement no. 776403 ExoplANETS-A). A.S. and
St.M. acknowledge funding from the Programme National de Planetologie
(PNP). A.R.G.S. acknowledges the support from the FCT through national
funds and FEDER through COMPETE2020 (UIDB/04434/2020 &
UIDP/04434/2020) and the support from the FCT through the work
contract No. 2020.02480.CEECIND/CP1631/CT0001. Sa.M. acknowledges
support from the Spanish Ministry of Science and Innovation (MICINN)
with the Ramon y Cajal fellowship no. RYC-2015-17697 and through AEI
under the Severo Ochoa Centres of Excellence Programme 2020-2023
(CEX2019- 000920-S). Sa.M. and D.G.R. acknowledge support from the
Spanish Ministry of Science and Innovation (MICINN) with the grant no.
PID2019-107187GB- I00. PGB acknowledges support by the Spanish
Ministry of Science and Innovation with the Ramon y Cajal fellowship
number RYC-2021-033137-I and the number MRR4032204. S.N.B acknowledges
support from PLATO ASI-INAF agreement n. 2015-019-R.1-2018. P.G.B.
acknowledges the financial support by NAWI Graz. The work presented
here was partially supported by the NASA grant NNX17AF27G. This paper
includes data collected by the Kepler mission and obtained from the
MAST data archive at the Space Telescope Science Institute (STScI).
Funding for the Kepler mission is provided by the NASA Science Mission
Directorate. STScI is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS 5-26555. This
research has made use of the NASA Exoplanet Archive, which is operated
by the California Institute of Technology, under contract with the
National Aeronautics and Space Administration under the Exoplanet
Exploration Program. This research was supported in part by the
National Science Foundation under Grant No. NSF PHY-1748958. The
authors acknowledge the participants of the Probes of Transport in
Stars (transtar21) KITP Program for the usefull discussions and
comments about this work. Software: AstroPy (Astropy Collaboration et
al., 2013A&A...558A..33A 2013A&A...558A..33A, 2018AJ....156..123A 2018AJ....156..123A), KADACS (Garcia et al.
2011MNRAS.414L...6G 2011MNRAS.414L...6G), ROOSTER (Breton et al. 2021A&A...647A.125B 2021A&A...647A.125B),
Matplotlib (Hunter 2007, Computing in Science & Engineering, 9, 90),
NumPy (van der Walt et al. 2011, CiSE, 13, 22), SciPy (Jones et al
2001, SciPy: Open source scientific tools for Python), Seaborn (Waskom
2021, Journal of Open Source Software, 6, 3021), pandas (Wes McKinney
2010, in Proceedings of the 9th Python in Science Conference, ed.
Stefan van der Walt & Jarrod Millman, 56-61 ; pandas development team
2020), ESPEM (Ahuir et al. 2021A&A...650A.126A 2021A&A...650A.126A).
(End) Patricia Vannier [CDS] 31-Oct-2023