Discovery of post-mass-transfer helium-burning red giants using asteroseismology
A star expands to become a red giant when it has fused all the hydrogen in its core into
helium. If the star is in a binary system, its envelope can overflow onto its companion or be …
helium. If the star is in a binary system, its envelope can overflow onto its companion or be …
Standing on the shoulders of giants: New mass and distance estimates for betelgeuse through combined evolutionary, asteroseismic, and hydrodynamic simulations …
We conduct a rigorous examination of the nearby red supergiant Betelgeuse by drawing on
the synthesis of new observational data and three different modeling techniques. Our …
the synthesis of new observational data and three different modeling techniques. Our …
First results on RR Lyrae stars with the TESS space telescope: untangling the connections between mode content, colors, and distances
Abstract The Transiting Exoplanet Survey Satellite (TESS) space telescope is collecting
continuous, high-precision optical photometry of stars throughout the sky, including …
continuous, high-precision optical photometry of stars throughout the sky, including …
Study of changes in the pulsation period of 148 Galactic Cepheid variables
G Csörnyei, L Szabados, L Molnár… - Monthly Notices of …, 2022 - academic.oup.com
Investigating period changes of classical Cepheids through the framework of O− C diagrams
provides a unique insight to the evolution and nature of these variable stars. In this work, the …
provides a unique insight to the evolution and nature of these variable stars. In this work, the …
The most metal-rich asymptotic giant branch stars
We present new stellar evolutionary sequences of very metal-rich stars evolved with the
Monash Stellar Structure code and with mesa. The Monash models include masses of 1–8 …
Monash Stellar Structure code and with mesa. The Monash models include masses of 1–8 …
A Buddy for Betelgeuse: Binarity as the Origin of the Long Secondary Period in α Orionis
We predict the existence of α Ori B, a low-mass companion orbiting Betelgeuse. This is
motivated by the presence of a 2170 day long secondary period (LSP) in Betelgeuse's …
motivated by the presence of a 2170 day long secondary period (LSP) in Betelgeuse's …
Semi-regular red giants as distance indicators-I. The period–luminosity relations of semi-regular variables revisited
M Trabucchi, N Mowlavi, T Lebzelter - Astronomy & Astrophysics, 2021 - aanda.org
Context. Semi-regular variables (SRVs) are similar to Miras in brightness, and they also
follow one or more period–luminosity relations (PLRs), though not necessarily the same one …
follow one or more period–luminosity relations (PLRs), though not necessarily the same one …
Hydrodynamic modelling of pulsation period decrease in the Mira-type variable T UMi
YA Fadeyev - Monthly Notices of the Royal Astronomical Society, 2022 - academic.oup.com
Pulsation period decrease during the initial stage of the thermal pulse in the helium-burning
shell of the Mira-type variable T UMi is investigated with numerical methods of stellar …
shell of the Mira-type variable T UMi is investigated with numerical methods of stellar …
Meandering periods and asymmetries in light curves of Miras: Observational evidence for low mass-loss rates
P Merchan-Benitez, S Uttenthaler… - Astronomy & …, 2023 - aanda.org
Context. Some Miras (long-period variables in late evolutionary stages) have meandering
pulsation periods and light-curve asymmetries, the causes of which are still unclear. Aims …
pulsation periods and light-curve asymmetries, the causes of which are still unclear. Aims …
Searching for Anomalies in the ZTF Catalog of Periodic Variable Stars
Periodic variables illuminate the physical processes of stars throughout their lifetime. Wide-
field surveys continue to increase our discovery rates of periodic variable stars. Automated …
field surveys continue to increase our discovery rates of periodic variable stars. Automated …