J/MNRAS/493/5871 TESS A and B stars and the Maia variables (Balona+, 2020)
Pulsation among TESS A and B stars and the Maia variables.
Balona L.A., Ozuyar D.
<Mon. Not. R. Astron. Soc., 493, 5871-5879 (2020)>
=2020MNRAS.493.5871B 2020MNRAS.493.5871B (SIMBAD/NED BibCode)
ADC_Keywords: Stars, B-type ; Stars, early-type ; Stars, variable ;
Effective temperatures ; Rotational velocities ; Spectral types ;
Optical
Keywords: stars: early-type - stars: oscillations
Abstract:
Classification of over 50000 TESS stars in sectors 1-18 has resulted
in the detection of 766 pulsating main-sequence B stars as well as
over 5000 δ Scuti, 2300 γ Doradus, and 114 roAp
candidates. Whereas it has been assumed that high-frequency pulsations
among B-type main-sequence stars are confined to the early B-type
β Cephei stars, the observations indicate that high frequencies
are to be found over the whole B-star range, eventually merging with
δ Scuti stars. The cool B stars pulsating in high frequencies
are called Maia variables. It is shown that Maia variables are not
rapidly rotating and thus cannot be β Cephei pulsators that
appear to have lower temperatures due to gravity darkening. In the
region where β Cephei variables are found, the proportion of
pulsating stars is larger and amplitudes are higher and a considerable
fraction pulsate in a single mode and low rotation rate. There is no
distinct region of slowly pulsating B stars (SPB stars). Stars
pulsating solely in low frequencies are found among all B stars. At
most, only one-third of B stars appear to pulsate. These results, as
well as the fact that a large fraction of A and B stars show
rotational modulation, indicate a need for a revision of current ideas
regarding stars with radiative envelopes.
Description:
Classification of B-type pulsating variables, their effective
temperatures and luminosities, projected rotational velocities and
spectral types are presented. The classification is based on visual
inspection of the light curve and periodogram. Effective temperatures
are from the literature and selected according to a list of priorities
depending on how they were measured. Only measurements with highest
priorities (listed) are used. The luminosities are derived from Gaia
DR2 parallaxes and a 3-D reddening model. The projected rotational
velocities are mean values from the literature. The spectral type is
representative from the literature.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 58 766 List of β Cep, SPB, and Maia stars in TESS
sectors 1-18
table2.dat 41 41 List of Maia stars with known projected
rotational velocities
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
IV/39 : TESS Input Catalog version 8.2 (TIC v8.2) (Paegert+, 2021)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 9 I9 --- TIC TESS Input Catalog identifier
11- 22 A12 --- VarType Variability classification (1)
24- 28 I5 K Teff Effective temperature
30 I1 --- Pr Priority code for effective temperature (G1)
32- 35 F4.2 [Lsun] logL Logarithm of the star luminosity (G2)
37- 39 I3 km/s vsini ? Mean projected rotational velocity
41- 58 A18 --- SpType Spectral type
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Note (1): Variability type as follows:
ACV = Rotational modulation due to chemical spots (A0 and later)
BCEP = Beta Cephei
EA = Algol-type eclipsing system
EB = Beta Lyrae-type eclipsing system
MAIA = Maia variable
ROT = Rotational variable
SPB = Slowly pulsating B star variable
SXARI = Rotational modulation due to chemical spots (B9 and earlier)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 9 I9 --- TIC TESS Input Catalog identifier
11- 15 I5 K Teff Effective temperature
17 I1 --- Pr Priority code for effective temperature (G1)
19- 22 F4.2 [Lsun] logL Logarithm of the star luminosity (G2)
24- 28 F5.1 km/s vsini Mean projected rotational velocity
30- 41 A12 --- SpType Spectral type
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Global Notes:
Note (G1): Source of Teff as follows:
1 = Spectroscopic modelling
2 = Stromgren or Geneva photometry
3 = UBV photometry
4 = BV photometry plus 3D reddening model
5 = Spectral classification
Note (G2): Stellar luminosities were derived from GaiaDR2 parallaxes
(Gaia Collaboration et al. 2018A&A...616A...1G 2018A&A...616A...1G, Cat. I/345)
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 15-May-2023