C.D.S. - SIMBAD4 rel 1.7 - 2020.07.16CEST15:59:36

2008A&A...492..815T - Astronomy and Astrophysics, volume 492, 815-821 (2008/12-4)

Time-resolved high-resolution spectroscopy of the bright pulsating subdwarf B star Balloon090100001.


Abstract (from CDS):

We have obtained, for the first time, a time-resolved high-resolution spectroscopic data set of the bright sdBV Balloon090100001. In the autumn of 2006 we gathered over 1600 time-resolved high-resolution spectra with the aim to identify the pulsation modes in Balloon090100001 by studying the line-profile variations. In this paper we present the results obtained from 842 spectra secured in August 2006, aiming to identify the dominant pulsation mode in this star. We phase fold the spectra onto the known dominant period of 2.80746mHz, to study the abundances and line-broadening as a function of pulsation phase. We find that the abundances do not stand out against those of other subdwarf B stars. Consequently, there is no way to demonstrate that the richness of the frequency spectrum and/or the high pulsation amplitudes are related to abundance effects. The abundances do not change with pulsational phase. The metal lines in Balloon090100001 are much broader than for non-pulsating subdwarfs, and during the cycle of the main pulsation the line broadening varies with ∼2.5km/s amplitude. Hence, we find clear evidence of pulsational broadening of the lines. We combine the information content of 56 narrow absorption lines through a cross-correlation technique, to create cross-correlation functions that for each individual pulsation phase approximate the average line-profile shape. The resulting profiles have a sufficient signal-to-noise ratio for a mode-identification analysis. From the cross-correlation analysis we find that the pulsation amplitude of the main mode decreased from 19km/s in 2004 to 14.5km/s in 2006. We present, for an sdB star, the first application of pulsation-mode identification based on line-profile variations of lines of heavy elements. To fit the line profiles we consider all modes with degree l≤2 and associated azimuthal order m, and we use a model of the pulsational surface-velocity field. The models with l=2 do not fit the profiles well, and consequently we can rule out quadrupole modes as the origin of the main pulsation mode in Balloon 090100001. Best fits are obtained from the model of a radial pulsation (l=0) and the model of a dipole pulsation (l=1).

Abstract Copyright:

Journal keyword(s): stars: subdwarfs - line: profiles - stars: early-type - stars: oscillations - stars: variables: general - stars: individual: Balloon090100001

CDS comments: Paragraph.1 KPD 1209+4401 is a misprint for KPD 2109+4401.

Simbad objects: 7

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Number of rows : 7

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
1 V* EO Cet HS* 01 23 43.2472884132 -05 05 45.831031643   12.21 12.65     sdOV+F4V 57 0
2 Feige 48 HS* 11 47 14.4977747924 +61 15 31.790488292   13.12 13.28     sdB 111 0
3 PG 1325+102 HS* 13 27 48.5602550889 +09 54 51.048576366   13.73 13.98 14.29   sdBO 52 1
4 V* NY Vir HS* 13 38 48.1466489725 -02 01 49.209465866   13.43 13.66 13.75   sdB1VIIHe1 191 1
5 PG 1605+072 HS* 16 08 03.6872880396 +07 04 28.747599362   12.53 12.83 13.18   sdB0.2VIHe3 121 0
6 KPD 2109+4401 HS* 21 11 47.6446188582 +44 13 50.621291301 12.14 13.11 13.30 13.64   sdB 62 0
7 Balloon 90100001 HS* 23 15 21.4810383697 +29 05 01.429272894   11.90 12.30     sdB 74 0

    Equat.    Gal    SGal    Ecl

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