J/PASP/134/H2001 Stellar obliquities in exoplanetary systems (Albrecht+, 2022)
Stellar obliquities in exoplanetary systems.
Albrecht S.H., Dawson R.I., Winn J.N.
<Publ. Astron. Soc. Pac. 134, H2001 (2022)>
=2022PASP..134h2001A 2022PASP..134h2001A (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Binaries, orbits ;
Optical
Keywords: planet hosting stars - stellar rotation - tidal interaction -
exoplanet dynamics - exoplanet formation - exoplanet migration
Abstract:
The rotation of a star and the revolutions of its planets are not
necessarily aligned. This article reviews the measurement techniques,
key findings, and theoretical interpretations related to the
obliquities (spin-orbit angles) of planet-hosting stars. The best
measurements are for stars with short-period giant planets, which have
been found on prograde, polar, and retrograde orbits. It seems likely
that dynamical processes such as planet-planet scattering and secular
perturbations are responsible for tilting the orbits of close-in giant
planets, just as those processes are implicated in exciting orbital
eccentricities. The observed dependence of the obliquity on orbital
separation, planet mass, and stellar structure suggests that in some
cases, tidal dissipation damps a star's obliquity within its
main-sequence lifetime. The situation is not as clear for stars with
smaller or wider-orbiting planets. Although the earliest measurements
of such systems tended to find low obliquities, some glaring
exceptions are now known in which the star's rotation is misaligned
with respect to the coplanar orbits of multiple planets. In addition,
statistical analyses based on projected rotation velocities and
photometric variability have found a broad range of obliquities for
F-type stars hosting compact multiple-planet systems. The results
suggest it is unsafe to assume that stars and their protoplanetary
disks are aligned. Primordial misalignments might be produced by
neighboring stars or more complex events that occur during the epoch
of planet formation.
Description:
Key properties of planets for which lambda, i, or both angles were
determined.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 127 24 Key parameters of systems with multiple transiting
planets for which lambda, i, or both were Determined
tablea1.dat 165 172 *Key properties of planets for which lambda, i,
or both angles were determined
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Note on tablea1.dat: All data are taken from TEPCat
(https://www.astro.keele.ac.uk/jkt/tepcat/)(Southworth et al., 2011) or in
the references in refs.dat
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Planet Planet name
13- 16 I4 K Teff Effective temperature
19- 21 I3 K e_Teff Error on Teff (lower value)
24- 26 I3 K E_Teff Error on Teff (upper value)
28- 32 F5.2 --- a/R Orbital separation
34 A1 --- --- [-]
35- 38 F4.2 --- e_a/R Error on a/R (lower value)
40 A1 --- --- [+]
41- 44 F4.2 --- E_a/R Error on a/R (upper value)
46- 50 F5.2 Rjup r Radius
52 A1 --- --- [-]
53- 56 F4.2 Rjup e_r Error on r (lower value)
58 A1 --- --- [+]
59- 62 F4.2 Rjup E_r Error on r (upper value)
64- 68 F5.1 deg lambda ?=- Position angle between the sky projections
of the line-of-sight inclinations of the
stellar and orbital angular momentum
vectors (1)
70 A1 --- --- [-]
71- 74 F4.1 deg e_lambda ? Error on lambda (lower value)
76 A1 --- --- [+]
77- 80 F4.1 deg E_lambda ? Error on lambda (upper value)
82- 85 F4.1 deg i ?=- Line-of-sight inclination of the
stellar ngular momentum vector
87 A1 --- --- [-]
88- 91 F4.1 deg e_i ? Error on i (lower value)
93 A1 --- --- [+]
94- 97 F4.1 deg E_i ? Error on i (upper value)
99-103 F5.1 deg psi ?=- Obliquity
105 A1 --- --- [-]
106-109 F4.1 deg e_psi ? Error on psi (lower value)
111 A1 --- --- [+]
112-115 F4.1 deg E_psi ? Error on psi (upper value)
117-118 I2 --- r_lambda ? Reference to the work from which we drew
the lambda measurement (2)
120-127 A8 --- Refs Reference(s) to works reporting additional
measurements of lambda or other system
parameters not taken from TEPCat (Southworth
et al., 2011, Cat. J/A+A/527/A8)
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Note (1): For the lambda measurements, we provide the parameters of the planet
for which the measurement was made.
Note (2): All data were taken from TEPCat (Southworth et al.,
2011A&A...527A...8S 2011A&A...527A...8S, Cat. J/A+A/527/A8) or the following references:
1 = Hirano et al., 2020ApJ...899L..13H 2020ApJ...899L..13H
2 = Albrecht et al., 2021ApJ...916L...1A 2021ApJ...916L...1A
3 = Martioli et al., 2020A&A...641L...1M 2020A&A...641L...1M
4 = Palle et al., 2020A&A...643A..25P 2020A&A...643A..25P
5 = Addison et al., 2021AJ....162..137A 2021AJ....162..137A, Cat. J/AJ/162/137
6 = Christiansen et al., 2017AJ....154..122C 2017AJ....154..122C, Cat. J/AJ/154/122
7 = Bourrier et al., 2021A&A...654A.152B 2021A&A...654A.152B
8 = Dalal et al., 2019A&A...631A..28D 2019A&A...631A..28D
9 = Mann et al., 2020AJ....160..179M 2020AJ....160..179M
10 = Dai et al., 2020AJ....160..193D 2020AJ....160..193D
11 = Zhou et al., 2018ApJ...860..101Z 2018ApJ...860..101Z
12 = Hjorth et al., 2019MNRAS.484.3522H 2019MNRAS.484.3522H
13 = Hjorth et al., 2021, PNAS, 118, 2017418118
14 = Wang et al., 2018AJ....155...70W 2018AJ....155...70W
15 = Albrecht et al., 2013ApJ...771...11A 2013ApJ...771...11A
16 = Campante et al., 2016ApJ...819...85C 2016ApJ...819...85C
17 = Benomar et al., 2014PASJ...66...94B 2014PASJ...66...94B
18 = Sanchis-Ojeda et al., 2012Natur.487..449S 2012Natur.487..449S
19 = Chaplin et al., 2013ARA&A..51..353C 2013ARA&A..51..353C
20 = Huber et al., 2013, Sci, 342, 331
21 = Hirano et al., 2012ApJ...759L..36H 2012ApJ...759L..36H
22 = Newton et al., 2021AJ....161...65N 2021AJ....161...65N, Cat. J/AJ/161/65
23 = Zhou et al., 2021AJ....161....2Z 2021AJ....161....2Z
24 = Wirth et al., 2021ApJ...917L..34W 2021ApJ...917L..34W
25 = Hirano et al., 2020ApJ...890L..27H 2020ApJ...890L..27H
26 = David et al., 2019AJ....158...79D 2019AJ....158...79D
27 = Johnson et al., 2022AJ....163..247J 2022AJ....163..247J, Cat. J/AJ/163/247
28 = Biddle et al., 2014MNRAS.443.1810B 2014MNRAS.443.1810B
29 = Gaidos et al., 2022MNRAS.509.2969G 2022MNRAS.509.2969G
30 = Feinstein et al., 2021AJ....162..213F 2021AJ....162..213F
31 = Sanchis-Ojeda et al., 2015ApJ...812L..11S 2015ApJ...812L..11S
32 = Wang et al., 2022ApJ...926L...8W 2022ApJ...926L...8W
33 = Hebrard et al., 2020A&A...640A..32H 2020A&A...640A..32H, Cat. J/A+A/640/A32
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Planet Planet name
18- 24 F7.2 --- a/R Orbital separation
27- 30 F4.2 --- e_a/R Error on a/R (lower value)
33- 36 F4.2 --- E_a/R Error on a/R (upper value)
38- 42 F5.2 Mjup m Mass
45- 48 F4.2 Mjup e_m ? Error on m (lower value)
51- 55 F5.2 Mjup E_m ? Error om m (upper value)
57- 60 F4.2 Rjup r Radius
63- 66 F4.2 Rjup e_r Error on r (lower value)
69- 72 F4.2 Rjup E_r Error on r (upper value)
74- 78 F5.3 --- e Ellipticity
81- 85 F5.3 --- e_e ? Error on e (lower value)
88- 92 F5.3 --- E_e ? Error on e (upper value)
94- 98 F5.1 deg lambda ?=- Position angle between the sky projections
of the line-of-sight inclinations of the
stellar and orbital angular momentum vectors
101-104 F4.1 deg e_lambda ? Error on lambda (lower value)
107-110 F4.1 deg E_lambda ? Error on lambda (upper value)
112-116 F5.1 deg i ?=- Line-of-sight inclination of the
stellar ngular momentum vector
119-122 F4.1 deg e_i ? Error on i (lower value)
125-128 F4.1 deg E_i ? Error on i (upper value)
130-134 F5.1 deg psi ?=- Obliquity
137-140 F4.1 deg e_psi ? Error on psi (lower value)
143-146 F4.1 deg E_psi ? Error on psi (upper value)
148-165 A18 --- Refs References for lambda or other system
parameters not taken from TEPCat (Southworth
et al., 2011, Cat. J/A+A/527/A8),
in refs.dat file
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 17-Jan-2023