The nature of the photometric variability of HgMn stars: a test of simulated light curves of phi Phe against the TESS data
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The nature of the photometric variability of HgMn stars : a test of simulated light curves of phi Phe against the TESS data. / Prvak, Milan; Krticka, Jiri; Korhonen, Heidi.
In: Monthly Notices of the Royal Astronomical Society, Vol. 492, No. 2, 02.2020, p. 1834-1840.Research output: Contribution to journal › Journal article › Research › peer-review
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TY - JOUR
T1 - The nature of the photometric variability of HgMn stars
T2 - a test of simulated light curves of phi Phe against the TESS data
AU - Prvak, Milan
AU - Krticka, Jiri
AU - Korhonen, Heidi
PY - 2020/2
Y1 - 2020/2
N2 - The inhomogeneous surface distribution of heavy elements is known to cause periodic light variability of magnetic chemically peculiar stars. It is unclear to what extent the same paradigm applies to mercury-manganese (HgMn)stars. We aim to model the photometric variability of the HgMn star phi Phe using abundance maps obtained from high-resolution spectroscopy and to study how this variability evolves with time. We compute a grid of ATLAS12 model atmospheres and the corresponding SYNSPEC synthetic spectra. Interpolating within this grid and integrating the specific intensity over the visible stellar surface at different rotational phases, we obtain theoretical light curves of the star. We predict the variability of phi Phe in the ultraviolet and in the visible spectral regions with amplitude of the order of millimagnitudes, mainly caused by absorption in lines of yttrium, chromium, and titanium. We also show how this variability is affected by changes of the distribution of the heavy elements over time. The main characteristics of the predicted light variability of phi Phe correspond roughly to the variability of the star observed with the Transiting Exoplanet Survey Satellite (TESS).
AB - The inhomogeneous surface distribution of heavy elements is known to cause periodic light variability of magnetic chemically peculiar stars. It is unclear to what extent the same paradigm applies to mercury-manganese (HgMn)stars. We aim to model the photometric variability of the HgMn star phi Phe using abundance maps obtained from high-resolution spectroscopy and to study how this variability evolves with time. We compute a grid of ATLAS12 model atmospheres and the corresponding SYNSPEC synthetic spectra. Interpolating within this grid and integrating the specific intensity over the visible stellar surface at different rotational phases, we obtain theoretical light curves of the star. We predict the variability of phi Phe in the ultraviolet and in the visible spectral regions with amplitude of the order of millimagnitudes, mainly caused by absorption in lines of yttrium, chromium, and titanium. We also show how this variability is affected by changes of the distribution of the heavy elements over time. The main characteristics of the predicted light variability of phi Phe correspond roughly to the variability of the star observed with the Transiting Exoplanet Survey Satellite (TESS).
KW - radiative transfer
KW - stars: atmospheres
KW - stars: chemically peculiar
KW - stars: early-type
KW - stars: individual: phi Phe
KW - stars: variables: general
U2 - 10.1093/mnras/stz3564
DO - 10.1093/mnras/stz3564
M3 - Journal article
VL - 492
SP - 1834
EP - 1840
JO - Royal Astronomical Society. Monthly Notices
JF - Royal Astronomical Society. Monthly Notices
SN - 0035-8711
IS - 2
ER -
ID: 248237061