TY - JOUR
T1 - Hats-18B
T2 - An extreme short-period massive transiting planet spinning up its star
AU - Penev, K.
AU - Hartman, J. D.
AU - Bakos, G.
AU - Ciceri, S.
AU - Brahm, R.
AU - Bayliss, D.
AU - Bento, J.
AU - Jordán, A.
AU - Csubry, Z.
AU - Bhatti, W.
AU - De Val-Borro, M.
AU - Espinoza, N.
AU - Zhou, G.
AU - Mancini, L.
AU - Rabus, M.
AU - Suc, V.
AU - Henning, T.
AU - Schmidt, B.
AU - Noyes, R. W.
AU - Lázár, J.
AU - Papp, I.
AU - Sári, P.
N1 - Publisher Copyright:
© 2016. The American Astronomical Society. All rights reserved.
PY - 2016/11
Y1 - 2016/11
N2 - We report the discovery by the HATSouth network of HATS-18b: a 1.980 ± 0.077 MJ, - 1.337-0.049 +0.102 RJ planet in a 0.8378 day orbit, around a solar analog star (mass 1.037 ± 0.047 M⊙ and radius - 1.020-0.031 +0.057 R⊙) with V=14.067±0.040 mag. The high planet mass, combined with its short orbital period, implies strong tidal coupling between the planetary orbit and the star. In fact, given its inferred age, HATS-18 shows evidence of significant tidal spin up, which together with WASP-19 (a very similar system) allows us to constrain the tidal quality factor for Sun-like stars to be in the range of 6.5≲log10(Q∗/k2)≲7 even after allowing for extremely pessimistic model uncertainties. In addition, the HATS-18 system is among the best systems (and often the best system) for testing a multitude of star-planet interactions, be they gravitational, magnetic, or radiative, as well as planet formation and migration theories.
AB - We report the discovery by the HATSouth network of HATS-18b: a 1.980 ± 0.077 MJ, - 1.337-0.049 +0.102 RJ planet in a 0.8378 day orbit, around a solar analog star (mass 1.037 ± 0.047 M⊙ and radius - 1.020-0.031 +0.057 R⊙) with V=14.067±0.040 mag. The high planet mass, combined with its short orbital period, implies strong tidal coupling between the planetary orbit and the star. In fact, given its inferred age, HATS-18 shows evidence of significant tidal spin up, which together with WASP-19 (a very similar system) allows us to constrain the tidal quality factor for Sun-like stars to be in the range of 6.5≲log10(Q∗/k2)≲7 even after allowing for extremely pessimistic model uncertainties. In addition, the HATS-18 system is among the best systems (and often the best system) for testing a multitude of star-planet interactions, be they gravitational, magnetic, or radiative, as well as planet formation and migration theories.
KW - planetary systems
KW - planets and satellites: detection
KW - planets and satellites: gaseous planets
KW - stars: individual (HATS-18)
KW - stars: rotation
KW - techniques: photometric
UR - http://www.scopus.com/inward/record.url?scp=84994545699&partnerID=8YFLogxK
U2 - 10.3847/0004-6256/152/5/127
DO - 10.3847/0004-6256/152/5/127
M3 - Article
AN - SCOPUS:84994545699
SN - 0004-6256
VL - 152
JO - Astronomical Journal
JF - Astronomical Journal
IS - 5
M1 - 127
ER -