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Title: THE WELL-ALIGNED ORBIT OF WASP-84b: EVIDENCE FOR DISK MIGRATION OF A HOT JUPITER

Abstract

We report the sky-projected orbital obliquity (spin–orbit angle) of WASP-84 b, a 0.69M{sub Jup} planet in an 8.52 day orbit around a G9V/K0V star, to be λ = −0.3 ± 1.7°. We obtain a true obliquity of ψ = 17.3 ± 7.7° from a measurement of the inclination of the stellar spin axis with respect to the sky plane. Due to the young age and the weak tidal forcing of the system, we suggest that the orbit of WASP-84b is unlikely to have both realigned and circularized from the misaligned and/or eccentric orbit likely to have arisen from high-eccentricity migration. Therefore we conclude that the planet probably migrated via interaction with the protoplanetary disk. This would make it the first “hot Jupiter” (P<10 d) to have been shown to have migrated via this pathway. Further, we argue that the distribution of obliquities for planets orbiting cool stars (T{sub eff} < 6250 K) suggests that high-eccentricity migration is an important pathway for the formation of short-orbit, giant planets.

Authors:
; ; ; ; ; ; ; ; ; ; ; ; ; ;  [1]
  1. N. Copernicus Astronomical Centre, Polish Academy of Sciences, Bartycka 18, 00-716, Warsaw (Poland)
Publication Date:
OSTI Identifier:
22364202
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal Letters; Journal Volume: 800; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; INCLINATION; JUPITER PLANET; ORBITS; PROTOPLANETS; SATELLITES; STABILITY; STAR EVOLUTION; STARS

Citation Formats

Anderson, D. R., Triaud, A. H. M. J., Turner, O. D., Brown, D. J. A., Clark, B. J. M., Smalley, B., Cameron, A. Collier, Doyle, A. P., Gillon, M., Hellier, C., Lovis, C., Maxted, P. F. L., Pollacco, D., Queloz, D., and Smith, A. M. S., E-mail: d.r.anderson@keele.ac.uk. THE WELL-ALIGNED ORBIT OF WASP-84b: EVIDENCE FOR DISK MIGRATION OF A HOT JUPITER. United States: N. p., 2015. Web. doi:10.1088/2041-8205/800/1/L9.
Anderson, D. R., Triaud, A. H. M. J., Turner, O. D., Brown, D. J. A., Clark, B. J. M., Smalley, B., Cameron, A. Collier, Doyle, A. P., Gillon, M., Hellier, C., Lovis, C., Maxted, P. F. L., Pollacco, D., Queloz, D., & Smith, A. M. S., E-mail: d.r.anderson@keele.ac.uk. THE WELL-ALIGNED ORBIT OF WASP-84b: EVIDENCE FOR DISK MIGRATION OF A HOT JUPITER. United States. doi:10.1088/2041-8205/800/1/L9.
Anderson, D. R., Triaud, A. H. M. J., Turner, O. D., Brown, D. J. A., Clark, B. J. M., Smalley, B., Cameron, A. Collier, Doyle, A. P., Gillon, M., Hellier, C., Lovis, C., Maxted, P. F. L., Pollacco, D., Queloz, D., and Smith, A. M. S., E-mail: d.r.anderson@keele.ac.uk. Tue . "THE WELL-ALIGNED ORBIT OF WASP-84b: EVIDENCE FOR DISK MIGRATION OF A HOT JUPITER". United States. doi:10.1088/2041-8205/800/1/L9.
@article{osti_22364202,
title = {THE WELL-ALIGNED ORBIT OF WASP-84b: EVIDENCE FOR DISK MIGRATION OF A HOT JUPITER},
author = {Anderson, D. R. and Triaud, A. H. M. J. and Turner, O. D. and Brown, D. J. A. and Clark, B. J. M. and Smalley, B. and Cameron, A. Collier and Doyle, A. P. and Gillon, M. and Hellier, C. and Lovis, C. and Maxted, P. F. L. and Pollacco, D. and Queloz, D. and Smith, A. M. S., E-mail: d.r.anderson@keele.ac.uk},
abstractNote = {We report the sky-projected orbital obliquity (spin–orbit angle) of WASP-84 b, a 0.69M{sub Jup} planet in an 8.52 day orbit around a G9V/K0V star, to be λ = −0.3 ± 1.7°. We obtain a true obliquity of ψ = 17.3 ± 7.7° from a measurement of the inclination of the stellar spin axis with respect to the sky plane. Due to the young age and the weak tidal forcing of the system, we suggest that the orbit of WASP-84b is unlikely to have both realigned and circularized from the misaligned and/or eccentric orbit likely to have arisen from high-eccentricity migration. Therefore we conclude that the planet probably migrated via interaction with the protoplanetary disk. This would make it the first “hot Jupiter” (P<10 d) to have been shown to have migrated via this pathway. Further, we argue that the distribution of obliquities for planets orbiting cool stars (T{sub eff} < 6250 K) suggests that high-eccentricity migration is an important pathway for the formation of short-orbit, giant planets.},
doi = {10.1088/2041-8205/800/1/L9},
journal = {Astrophysical Journal Letters},
number = 1,
volume = 800,
place = {United States},
year = {Tue Feb 10 00:00:00 EST 2015},
month = {Tue Feb 10 00:00:00 EST 2015}
}