The GAPS programme with HARPS-N at TNG: VII. Putting exoplanets in the stellar context: Magnetic activity and asteroseismology of τ Bootis A ∗ ∗ ∗

F. Borsa, G. Scandariato, M. Rainer, A. Bignamini, A. Maggio, E. Poretti, A. F. Lanza, M. P. Di Mauro, S. Benatti, K. Biazzo, A. S. Bonomo, M. Damasso, M. Esposito, R. Gratton, L. Affer, M. Barbieri, C. Boccato, R. U. Claudi, R. Cosentino, E. CovinoS. Desidera, A. F M Fiorenzano, D. Gandolfi, A. Harutyunyan, J. Maldonado, G. Micela, P. Molaro, E. Molinari, I. Pagano, I. Pillitteri, G. Piotto, Evgenya Shkolnik, R. Silvotti, R. Smareglia, J. Southworth, A. Sozzetti, B. Stelzer

Research output: Contribution to journalArticle

26 Citations (Scopus)

Abstract

Aims. We observed the τ Boo system with the HARPS-N spectrograph to test a new observational strategy aimed at jointly studying asteroseismology, the planetary orbit, and star-planet magnetic interaction. Methods. We collected high-cadence observations on 11 nearly consecutive nights and for each night averaged the raw FITS files using a dedicated software. In this way we obtained spectra with a high signal-to-noise ratio, used to study the variation of the Ca ii H&K lines and to have radial velocity values free from stellar oscillations, without losing the oscillations information. We developed a dedicated software to build a new custom mask that we used to refine the radial velocity determination with the HARPS-N pipeline and perform the spectroscopic analysis. Results. We updated the planetary ephemeris and showed the acceleration caused by the stellar binary companion. Our results on the stellar activity variation suggest the presence of a high-latitude plage during the time span of our observations. The correlation between the chromospheric activity and the planetary orbital phase remains unclear. Solar-like oscillations are detected in the radial velocity time series: we estimated asteroseismic quantities and found that they agree well with theoretical predictions. Our stellar model yields an age of 0.9 ± 0.5 Gyr for τ Boo and further constrains the value of the stellar mass to 1.38 ± 0.05 M.

Original languageEnglish (US)
Article numberA64
JournalAstronomy and Astrophysics
Volume578
DOIs
StatePublished - Jun 1 2015
Externally publishedYes

Fingerprint

asteroseismology
extrasolar planets
radial velocity
oscillation
night
stellar oscillations
planetary orbits
stellar activity
computer programs
solar oscillations
software
faculae
K lines
stellar models
spectroscopic analysis
stellar mass
files
polar regions
signal-to-noise ratio
spectrographs

Keywords

  • Asteroseismology
  • Planetary systems
  • Stars: activity
  • Stars: individual:τBoo
  • Techniques: spectroscopic

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

The GAPS programme with HARPS-N at TNG : VII. Putting exoplanets in the stellar context: Magnetic activity and asteroseismology of τ Bootis A ∗ ∗ ∗. / Borsa, F.; Scandariato, G.; Rainer, M.; Bignamini, A.; Maggio, A.; Poretti, E.; Lanza, A. F.; Di Mauro, M. P.; Benatti, S.; Biazzo, K.; Bonomo, A. S.; Damasso, M.; Esposito, M.; Gratton, R.; Affer, L.; Barbieri, M.; Boccato, C.; Claudi, R. U.; Cosentino, R.; Covino, E.; Desidera, S.; Fiorenzano, A. F M; Gandolfi, D.; Harutyunyan, A.; Maldonado, J.; Micela, G.; Molaro, P.; Molinari, E.; Pagano, I.; Pillitteri, I.; Piotto, G.; Shkolnik, Evgenya; Silvotti, R.; Smareglia, R.; Southworth, J.; Sozzetti, A.; Stelzer, B.

In: Astronomy and Astrophysics, Vol. 578, A64, 01.06.2015.

Research output: Contribution to journalArticle

Borsa, F, Scandariato, G, Rainer, M, Bignamini, A, Maggio, A, Poretti, E, Lanza, AF, Di Mauro, MP, Benatti, S, Biazzo, K, Bonomo, AS, Damasso, M, Esposito, M, Gratton, R, Affer, L, Barbieri, M, Boccato, C, Claudi, RU, Cosentino, R, Covino, E, Desidera, S, Fiorenzano, AFM, Gandolfi, D, Harutyunyan, A, Maldonado, J, Micela, G, Molaro, P, Molinari, E, Pagano, I, Pillitteri, I, Piotto, G, Shkolnik, E, Silvotti, R, Smareglia, R, Southworth, J, Sozzetti, A & Stelzer, B 2015, 'The GAPS programme with HARPS-N at TNG: VII. Putting exoplanets in the stellar context: Magnetic activity and asteroseismology of τ Bootis A ∗ ∗ ∗', Astronomy and Astrophysics, vol. 578, A64. https://doi.org/10.1051/0004-6361/201525741
Borsa, F. ; Scandariato, G. ; Rainer, M. ; Bignamini, A. ; Maggio, A. ; Poretti, E. ; Lanza, A. F. ; Di Mauro, M. P. ; Benatti, S. ; Biazzo, K. ; Bonomo, A. S. ; Damasso, M. ; Esposito, M. ; Gratton, R. ; Affer, L. ; Barbieri, M. ; Boccato, C. ; Claudi, R. U. ; Cosentino, R. ; Covino, E. ; Desidera, S. ; Fiorenzano, A. F M ; Gandolfi, D. ; Harutyunyan, A. ; Maldonado, J. ; Micela, G. ; Molaro, P. ; Molinari, E. ; Pagano, I. ; Pillitteri, I. ; Piotto, G. ; Shkolnik, Evgenya ; Silvotti, R. ; Smareglia, R. ; Southworth, J. ; Sozzetti, A. ; Stelzer, B. / The GAPS programme with HARPS-N at TNG : VII. Putting exoplanets in the stellar context: Magnetic activity and asteroseismology of τ Bootis A ∗ ∗ ∗. In: Astronomy and Astrophysics. 2015 ; Vol. 578.
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abstract = "Aims. We observed the τ Boo system with the HARPS-N spectrograph to test a new observational strategy aimed at jointly studying asteroseismology, the planetary orbit, and star-planet magnetic interaction. Methods. We collected high-cadence observations on 11 nearly consecutive nights and for each night averaged the raw FITS files using a dedicated software. In this way we obtained spectra with a high signal-to-noise ratio, used to study the variation of the Ca ii H&K lines and to have radial velocity values free from stellar oscillations, without losing the oscillations information. We developed a dedicated software to build a new custom mask that we used to refine the radial velocity determination with the HARPS-N pipeline and perform the spectroscopic analysis. Results. We updated the planetary ephemeris and showed the acceleration caused by the stellar binary companion. Our results on the stellar activity variation suggest the presence of a high-latitude plage during the time span of our observations. The correlation between the chromospheric activity and the planetary orbital phase remains unclear. Solar-like oscillations are detected in the radial velocity time series: we estimated asteroseismic quantities and found that they agree well with theoretical predictions. Our stellar model yields an age of 0.9 ± 0.5 Gyr for τ Boo and further constrains the value of the stellar mass to 1.38 ± 0.05 M.",
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T1 - The GAPS programme with HARPS-N at TNG

T2 - VII. Putting exoplanets in the stellar context: Magnetic activity and asteroseismology of τ Bootis A ∗ ∗ ∗

AU - Borsa, F.

AU - Scandariato, G.

AU - Rainer, M.

AU - Bignamini, A.

AU - Maggio, A.

AU - Poretti, E.

AU - Lanza, A. F.

AU - Di Mauro, M. P.

AU - Benatti, S.

AU - Biazzo, K.

AU - Bonomo, A. S.

AU - Damasso, M.

AU - Esposito, M.

AU - Gratton, R.

AU - Affer, L.

AU - Barbieri, M.

AU - Boccato, C.

AU - Claudi, R. U.

AU - Cosentino, R.

AU - Covino, E.

AU - Desidera, S.

AU - Fiorenzano, A. F M

AU - Gandolfi, D.

AU - Harutyunyan, A.

AU - Maldonado, J.

AU - Micela, G.

AU - Molaro, P.

AU - Molinari, E.

AU - Pagano, I.

AU - Pillitteri, I.

AU - Piotto, G.

AU - Shkolnik, Evgenya

AU - Silvotti, R.

AU - Smareglia, R.

AU - Southworth, J.

AU - Sozzetti, A.

AU - Stelzer, B.

PY - 2015/6/1

Y1 - 2015/6/1

N2 - Aims. We observed the τ Boo system with the HARPS-N spectrograph to test a new observational strategy aimed at jointly studying asteroseismology, the planetary orbit, and star-planet magnetic interaction. Methods. We collected high-cadence observations on 11 nearly consecutive nights and for each night averaged the raw FITS files using a dedicated software. In this way we obtained spectra with a high signal-to-noise ratio, used to study the variation of the Ca ii H&K lines and to have radial velocity values free from stellar oscillations, without losing the oscillations information. We developed a dedicated software to build a new custom mask that we used to refine the radial velocity determination with the HARPS-N pipeline and perform the spectroscopic analysis. Results. We updated the planetary ephemeris and showed the acceleration caused by the stellar binary companion. Our results on the stellar activity variation suggest the presence of a high-latitude plage during the time span of our observations. The correlation between the chromospheric activity and the planetary orbital phase remains unclear. Solar-like oscillations are detected in the radial velocity time series: we estimated asteroseismic quantities and found that they agree well with theoretical predictions. Our stellar model yields an age of 0.9 ± 0.5 Gyr for τ Boo and further constrains the value of the stellar mass to 1.38 ± 0.05 M.

AB - Aims. We observed the τ Boo system with the HARPS-N spectrograph to test a new observational strategy aimed at jointly studying asteroseismology, the planetary orbit, and star-planet magnetic interaction. Methods. We collected high-cadence observations on 11 nearly consecutive nights and for each night averaged the raw FITS files using a dedicated software. In this way we obtained spectra with a high signal-to-noise ratio, used to study the variation of the Ca ii H&K lines and to have radial velocity values free from stellar oscillations, without losing the oscillations information. We developed a dedicated software to build a new custom mask that we used to refine the radial velocity determination with the HARPS-N pipeline and perform the spectroscopic analysis. Results. We updated the planetary ephemeris and showed the acceleration caused by the stellar binary companion. Our results on the stellar activity variation suggest the presence of a high-latitude plage during the time span of our observations. The correlation between the chromospheric activity and the planetary orbital phase remains unclear. Solar-like oscillations are detected in the radial velocity time series: we estimated asteroseismic quantities and found that they agree well with theoretical predictions. Our stellar model yields an age of 0.9 ± 0.5 Gyr for τ Boo and further constrains the value of the stellar mass to 1.38 ± 0.05 M.

KW - Asteroseismology

KW - Planetary systems

KW - Stars: activity

KW - Stars: individual:τBoo

KW - Techniques: spectroscopic

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