J/A+A/690/A379 Obliquities of exoplanet host stars (Knudstrup+, 2024)
Obliquities of exoplanet host stars. Nineteen new and updated measurements,
and trends in the sample of 205 measurements.
Knudstrup E., Albrecht S.H., Winn J.N., Gandolfi D., Zanazzi J.,
Persson C.M., Fridlund M., Marcussen M.L., Chontos A., Keniger M.A.F.,
Eisner N.L., Bieryla A., Isaacson H., Howard A.W., Hirsch L.A., Murgas F.,
Narita N., Palle E., Kawai Y., Baker D.
<Astron. Astrophys. 690, A379 (2024)>
=2024A&A...690A.379K 2024A&A...690A.379K (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Radial velocities ;
Optical
Keywords: planets and satellites: dynamical evolution and stability -
planets and satellites: formation - planet-star interactions
Abstract:
Measurements of the obliquities in exoplanet systems have revealed
some remarkable architectures, some of which are very different
from the Solar System. Nearly 200 obliquity measurements have been
obtained through observations of the Rossiter-McLaughlin (RM) effect.
Here we report on observations of 19 planetary systems that led to 17
clear detections of the RM effect and 2 less secure detections. After
adding the new measurements to the tally, we use the entire collection
of RM measurements to investigate four issues that have arisen in the
literature. i) Does the obliquity distribution show a peak at
approximately 90°? We find tentative evidence that such a peak
does exist when restricting attention to the sample of sub-Saturn
planets and hot Jupiters orbiting F stars. ii) Are high obliquities
associated with high eccentricities? We find the association to be
weaker than previously reported, and that a stronger association
exists between obliquity and orbital separation, possibly due to tidal
obliquity damping at small separations. iii) How low are the lowest
known obliquities? Among hot Jupiters around cool stars, we find the
dispersion to be 1.4±0.7°, smaller than the 6° obliquity of
the Sun, which serves as additional evidence for tidal damping. iv)
What are the obliquities of stars with compact and flat systems of
multiple planets? We find that they generally have obliquities lower
than 10°, with several remarkable exceptions possibly caused by
wide-orbiting stellar or planetary companions.
Description:
Table containing all radial velocities (RVs) used with targets,
instruments, timestamps, RVs, and errors. Timestamps are given in
BJD_TDB, RVs and errors are given in m/s.
Instruments are assigned the following indices:
0 = FIES, 1 = FIES+, 2 = HARPS-N, 3 = ESPRESSO
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 46 18 List of studied stars
rv.dat 49 440 Radial velocity table
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Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Star name
11- 12 I2 h RAh Simbad right ascension (J2000)
14- 15 I2 min RAm Simbad right ascension (J2000)
17- 21 F5.2 s RAs Simbad right ascension (J2000)
23 A1 --- DE- Simbad declination sign (J2000)
24- 25 I2 deg DEd Simbad declination (J2000)
27- 28 I2 arcmin DEm Simbad declination (J2000)
30- 33 F4.1 arcsec DEs Simbad declination (J2000)
35- 36 I2 --- N Number of radial velocity values
38- 46 A9 --- SName Simbad name
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Byte-by-byte Description of file: rv.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Target [0/17] Target number
4 I1 --- Inst [0/3] Instrument (1)
6- 21 F16.8 d BJD Barycentric Julian date (TDB)
23- 32 F10.3 m/s RV Radial velocity
34- 39 F6.3 m/s e_RV Radial velocity error
41- 49 A9 --- Name Star name
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Note (1): Instrument code as follows:
0 = FIES
1 = FIES+
2 = HARPS-N
3 = ESPRESSO
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Acknowledgements:
Emil Knudstrup, emil.knudstrup(at)chalmers.se
(End) Patricia Vannier [CDS] 20-Aug-2024