Revisiting the pulsational characteristics of the exoplanet host star β Pictoris

被引：26

作者：

Zwintz, K. ^{[1
]}

Reese, D. R. ^{[2
]}

Neiner, C. ^{[2
]}

Pigulski, A. ^{[3
]}

Kuschnig, R. ^{[4
]}

Muellner, M. ^{[1
]}

Zieba, S. ^{[1
]}

Abe, L. ^{[5
]}

Guillot, T. ^{[5
]}

Handler, G. ^{[6
]}

Kenworthy, M. ^{[7
]}

Stuik, R. ^{[7
]}

Moffat, A. F. J. ^{[8
,9
]}

Popowicz, A. ^{[10
]}

Rucinski, S. M. ^{[11
]}

Wade, G. A. ^{[12
]}

Weiss, W. W. ^{[13
]}

Bailey, J. I., III ^{[14
]}

Crawford, S. ^{[15
,16
]}

Ireland, M. ^{[17
]}

Lomberg, B. ^{[16
,18
]}

Mamajek, E. E. ^{[19
,20
]}

Mellon, S. N. ^{[20
]}

Talens, G. J. ^{[7
,21
]}

机构：

[1] Univ Innsbruck, Inst Astro & Teilchenphys, Tech Str 25, A-6020 Innsbruck, Austria

[2] Univ Paris Diderot, Univ PSL, Sorbonne Univ, LESIA,Observ Paris,CNRS,Sorbonne Paris Cite, 5 Pl Jules Janssen, F-92195 Meudon, France

[3] Uniwersytet Wroclawski, Inst Astron, Kopernika 11, PL-51622 Wroclaw, Poland

[4] Graz Univ Technol, Inst Kommunikationsnetze & Satellitenkommunikat, Inffeldgasse 12, A-8010 Graz, Austria

[5] Univ Cote dAzur, Observ Cote dAzur, CNRS, Lab Lagrange, CS 34229, F-06304 Nice 4, France

[6] Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland

[7] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands

[8] Univ Montreal, Dept Phys, CP 6128,Succursale Ctr Ville, Montreal, PQ H3C 3J7, Canada

[9] CRAQ, Montreal, PQ H3C 3J7, Canada

[10] Silesian Tech Univ, Inst Automat Control, Akad 16, Gliwice, Poland

[11] Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada

[12] Royal Mil Coll Canada, Dept Phys & Space Sci, POB 17000, Kingston, ON K7K 7B4, Canada

[13] Univ Wien, Inst Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria

[14] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93111 USA

[15] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

[16] South African Astron Observ, Observ Rd, ZA-7700 Cape Town, South Africa

[17] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia

[18] Univ Cape Town, Dept Astron, ZA-7700 Cape Town, South Africa

[19] CALTECH, Jet Prop Lab, M-S 321-100,4800 Oak Grove Dr, Pasadena, CA 91109 USA

[20] Univ Rochester, Dept Phys & Astron, 500 Wilson Blvd, Rochester, NY 14627 USA

[21] Univ Montreal, Inst Rech Exoplanetes, Dept Phys, Montreal, PQ H3C 3J7, Canada

来源：

ASTRONOMY & ASTROPHYSICS | 2019年 / 627卷

基金：

加拿大自然科学与工程研究理事会; 美国国家航空航天局; 澳大利亚研究理事会;

关键词：

asteroseismology; stars: individual: beta Pictoris; stars: interiors; stars: variables: delta Scuti; stars: magnetic field; MAIN-SEQUENCE STARS; DELTA-SCUTI STARS; MAGNETIC-FIELD; NEARBY STARS; AP STARS; DISCOVERY; GRAVITY; AGE; ASTEROSEISMOLOGY; SPECTROSCOPY;

D O I：

10.1051/0004-6361/201834744

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Exoplanet properties crucially depend on the parameters of their host stars: more accurate stellar parameters yield more accurate exoplanet characteristics. When the exoplanet host star shows pulsations, asteroseismology can be used for an improved description of the stellar parameters. Aims. We aim to revisit the pulsational properties of beta Pic and identify its pulsation modes from normalized amplitudes in five different passbands. We also investigate the potential presence of a magnetic field. Methods. We conducted a frequency analysis using three seasons of BRITE-Constellation observations in the two BRITE filters, the about 620-day-long bRing light curve, and the nearly 8-year-long SMEI photometric time series. We calculated normalized amplitudes using all passbands and including previously published values obtained from ASTEP observations. We investigated the magnetic properties of beta Pic using spectropo-larimetric observations conducted with the HARPSpol instrument. Using 2D rotating models, we fit the normalized amplitudes and frequencies through Monte Carlo Markov chains. Results. We identify 15 pulsation frequencies in the range from 34 to 55 d(-1), where two, F13 at 53.6917 d(-1) and F11 at 50.4921 d(-1), display clear amplitude variability. We use the normalized amplitudes in up to five passbands to identify the modes as three l = 1, six l = 2; and six l = 3 modes. beta Pic is shown to be non-magnetic with an upper limit of the possible undetected dipolar field of 300 Gauss. Conclusions. Multiple fits to the frequencies and normalized amplitudes are obtained, including one with a near equator-on inclination for beta Pic, which corresponds to our expectations based on the orbital inclination of beta Pic b and the orientation of the circumstellar disk. This solution leads to a rotation rate of 27% of the Keplerian breakup velocity, a radius of 1.497 +/- 0.025 R-circle dot, and a mass of 1.797 +/- 0.035 M-circle dot. The similar to 2% errors in radius and mass do not account for uncertainties in the models and a potentially erroneous mode-identification.

引用

页数：25

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