Data Analysis of Bright Main-Sequence A- and B-type Stars Observed Using the TESS and BRITE Spacecraft. (arXiv:2008.12661v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Guzik_J/0/1/0/all/0/1">Joyce A. Guzik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jackiewicz_J/0/1/0/all/0/1">Jason Jackiewicz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pigulski_A/0/1/0/all/0/1">Andrzej Pigulski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Catanzaro_G/0/1/0/all/0/1">Giovanni Catanzaro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soukup_M/0/1/0/all/0/1">Michael S. Soukup</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaulme_P/0/1/0/all/0/1">Patrick Gaulme</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Handler_G/0/1/0/all/0/1">Gerald Handler</a>, the <a href="http://arxiv.org/find/astro-ph/1/au:+Team_BRITE/0/1/0/all/0/1">BRITE Team</a>
During the last two years we have received long time-series photometric
observations of bright (V mag < 8) main-sequence A- and B-type stars observed
by the NASA TESS spacecraft and the Austria-Poland-Canada BRITE satellites.
Using TESS observations of metallic-line A (Am) stars having peculiar element
abundances, our goal is to determine whether and why these stars pulsate in
multiple radial and non-radial modes, as do the delta Scuti stars in the same
region of the H-R diagram. The BRITE data were requested to investigate
pulsations in bright (V around 6 mag) A- and B-type stars in the Cygnus-Lyra
field of view that had been proposed for observations during the now-retired
NASA Kepler mission.
Of the 21 (out of 62 proposed) Am stars observed by TESS so far, we find one
delta Sct star and two delta Sct / gamma Dor hybrid candidates. Of the
remaining stars, we find three gamma Dor candidates, six stars showing
photometric variations that may or may not be associated with pulsations, and
eight stars without apparent significant photometric variability. For the A-
and B-type stars observed by BRITE, one star (HR 7403) shows low amplitude low
frequency modes that likely are associated with its B(emission) star
properties; one star (HR 7179) shows SPB variability that is also found in
prior Kepler data, and two stars (HR 7284 and HR 7591) show no variability in
BRITE data, although very low amplitude variability was found in TESS or Kepler
data. For the TESS and BRITE targets discussed here, follow-up ground- and
space-based photometric and spectroscopic observations combined with stellar
modeling will be needed to constrain stellar parameters and to understand the
nature of the variability.
During the last two years we have received long time-series photometric
observations of bright (V mag < 8) main-sequence A- and B-type stars observed
by the NASA TESS spacecraft and the Austria-Poland-Canada BRITE satellites.
Using TESS observations of metallic-line A (Am) stars having peculiar element
abundances, our goal is to determine whether and why these stars pulsate in
multiple radial and non-radial modes, as do the delta Scuti stars in the same
region of the H-R diagram. The BRITE data were requested to investigate
pulsations in bright (V around 6 mag) A- and B-type stars in the Cygnus-Lyra
field of view that had been proposed for observations during the now-retired
NASA Kepler mission.
Of the 21 (out of 62 proposed) Am stars observed by TESS so far, we find one
delta Sct star and two delta Sct / gamma Dor hybrid candidates. Of the
remaining stars, we find three gamma Dor candidates, six stars showing
photometric variations that may or may not be associated with pulsations, and
eight stars without apparent significant photometric variability. For the A-
and B-type stars observed by BRITE, one star (HR 7403) shows low amplitude low
frequency modes that likely are associated with its B(emission) star
properties; one star (HR 7179) shows SPB variability that is also found in
prior Kepler data, and two stars (HR 7284 and HR 7591) show no variability in
BRITE data, although very low amplitude variability was found in TESS or Kepler
data. For the TESS and BRITE targets discussed here, follow-up ground- and
space-based photometric and spectroscopic observations combined with stellar
modeling will be needed to constrain stellar parameters and to understand the
nature of the variability.
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