Activity induced variation in spin-orbit angles as derived from Rossiter-McLaughlin measurements
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 h...
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2018
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| Acceso en línea: | https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v619_n_p_Oshagh http://hdl.handle.net/20.500.12110/paper_00046361_v619_n_p_Oshagh |
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paper:paper_00046361_v619_n_p_Oshagh2023-06-08T14:28:26Z Activity induced variation in spin-orbit angles as derived from Rossiter-McLaughlin measurements Planets and satellites: Detection Planets and satellites: Fundamental parameters Stars: Activity Starspots Techniques: Photometric Techniques: Radial velocities Astrophysics Photometry Planets Satellites Stars Planets and satellites: detections Planets and satellites: fundamental parameters Stars: activity Starspots Techniques: photometric Techniques: radial velocities Orbits 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. © 2018 ESO. 2018 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v619_n_p_Oshagh http://hdl.handle.net/20.500.12110/paper_00046361_v619_n_p_Oshagh |
| institution |
Universidad de Buenos Aires |
| institution_str |
I-28 |
| repository_str |
R-134 |
| collection |
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) |
| topic |
Planets and satellites: Detection Planets and satellites: Fundamental parameters Stars: Activity Starspots Techniques: Photometric Techniques: Radial velocities Astrophysics Photometry Planets Satellites Stars Planets and satellites: detections Planets and satellites: fundamental parameters Stars: activity Starspots Techniques: photometric Techniques: radial velocities Orbits |
| spellingShingle |
Planets and satellites: Detection Planets and satellites: Fundamental parameters Stars: Activity Starspots Techniques: Photometric Techniques: Radial velocities Astrophysics Photometry Planets Satellites Stars Planets and satellites: detections Planets and satellites: fundamental parameters Stars: activity Starspots Techniques: photometric Techniques: radial velocities Orbits Activity induced variation in spin-orbit angles as derived from Rossiter-McLaughlin measurements |
| topic_facet |
Planets and satellites: Detection Planets and satellites: Fundamental parameters Stars: Activity Starspots Techniques: Photometric Techniques: Radial velocities Astrophysics Photometry Planets Satellites Stars Planets and satellites: detections Planets and satellites: fundamental parameters Stars: activity Starspots Techniques: photometric Techniques: radial velocities Orbits |
| description |
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. © 2018 ESO. |
| title |
Activity induced variation in spin-orbit angles as derived from Rossiter-McLaughlin measurements |
| title_short |
Activity induced variation in spin-orbit angles as derived from Rossiter-McLaughlin measurements |
| title_full |
Activity induced variation in spin-orbit angles as derived from Rossiter-McLaughlin measurements |
| title_fullStr |
Activity induced variation in spin-orbit angles as derived from Rossiter-McLaughlin measurements |
| title_full_unstemmed |
Activity induced variation in spin-orbit angles as derived from Rossiter-McLaughlin measurements |
| title_sort |
activity induced variation in spin-orbit angles as derived from rossiter-mclaughlin measurements |
| publishDate |
2018 |
| url |
https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v619_n_p_Oshagh http://hdl.handle.net/20.500.12110/paper_00046361_v619_n_p_Oshagh |
| _version_ |
1768542718396465152 |