2018A&A...619A.150O


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.16CET01:31:56

2018A&A...619A.150O - Astronomy and Astrophysics, volume 619A, 150-150 (2018/11-1)

Activity induced variation in spin-orbit angles as derived from Rossiter-McLaughlin measurements.

OSHAGH M., TRIAUD A.H.M.J., BURDANOV A., FIGUEIRA P., REINERS A., SANTOS N.C., FARIA J., BOUE G., DIAZ R.F., DREIZLER S., BOLDT S., DELREZ L., DUCROT E., GILLON M., GUZMAN MESA A., JEHIN E., KHALAFINEJAD S., KOHL S., SERRANO L. and UDRY S.

Abstract (from CDS):

One of the most powerful methods used to estimate sky-projected spin-orbit angles of exoplanetary systems is through a spectroscopic transit observation known as the RossiterMcLaughlin (RM) effect. So far mostly single RM observations have been used to estimate the spin-orbit angle, and thus there have been no studies regarding the variation of estimated spin-orbit angle from transit to transit. Stellar activity can alter the shape of photometric transit light curves and in a similar way they can deform the RM signal. In this paper we present several RM observations, obtained using the HARPS spectrograph, of known transiting planets that all transit extremely active stars, and by analyzing them individually we assess the variation in the estimated spin-orbit angle. Our results reveal that the estimated spin-orbit angle can vary significantly (up to ∼42°) from transit to transit, due to variation in the configuration of stellar active regions over different nights. This finding is almost two times larger than the expected variation predicted from simulations. We could not identify any meaningful correlation between the variation of estimated spin-orbit angles and the stellar magnetic activity indicators. We also investigated two possible approaches to mitigate the stellar activity influence on RM observations. The first strategy was based on obtaining several RM observations and folding them to reduce the stellar activity noise. Our results demonstrated that this is a feasible and robust way to overcome this issue. The second approach is based on acquiring simultaneous high-precision short-cadence photometric transit light curves using TRAPPIST/SPECULOOS telescopes, which provide more information about the stellar active region's properties and allow a better RM modeling.

Abstract Copyright: © ESO 2018

Journal keyword(s): planets and satellites: fundamental parameters - planets and satellites: detection - stars: activity - starspots - techniques: radial velocities - techniques: photometric

Simbad objects: 13

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Number of rows : 13

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 * rho01 Cnc e Pl 08 52 35.81093 +28 19 50.9511           ~ 358 1
2 WASP-19b Pl 09 53 40.0764883458 -45 39 33.055979403           ~ 217 1
3 WASP-19 LP* 09 53 40.0764883458 -45 39 33.055979403   13.05 12.31 12.12 11.35 G8V 120 1
4 WASP-41b Pl 12 42 28.4949324021 -30 38 23.527612553           ~ 25 1
5 WASP-41 * 12 42 28.4949324021 -30 38 23.527612553   12.36 11.63 11.39 10.78 G8V 35 1
6 EPIC 212756297.01 Pl 13 50 37.4100427817 -06 48 14.419877691           ~ 26 1
7 Qatar 2 * 13 50 37.4100427817 -06 48 14.419877691   14.0   13.45   K5V 41 1
8 CoRoT-2 * 19 27 06.4944821296 +01 23 01.357597206   13.422 12.568 12.204 11.49 G7V+K9V 201 2
9 CoRoT-2b Pl 19 27 06.4944821296 +01 23 01.357597206     12.57     ~ 170 1
10 WASP-6b Pl 23 12 37.7368657624 -22 40 26.277489164           ~ 86 1
11 WASP-6 * 23 12 37.7368657624 -22 40 26.277489164   12.90 11.91     G8V 64 1
12 WASP-52 * 23 13 58.7575814237 +08 45 40.571306719   12.9 12.0 12.03   K2V 36 1
13 WASP-52b Pl 23 13 58.76 +08 45 40.6           ~ 38 1

    Equat.    Gal    SGal    Ecl

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2019.11.16-01:31:56

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