Asteroseismology and Spectropolarimetry of the Exoplanet Host Star $\lambda$ Serpentis
Astron. J. 166, 167 (2023) The bright star $\lambda$ Ser hosts a hot Neptune with a minimum mass of 13.6 $M_\oplus$ and a 15.5 day orbit. It also appears to be a solar analog, with a mean rotation period of 25.8 days and surface differential rotation very similar to the Sun. We aim to characterize t...
Gespeichert in:
Hauptverfasser: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
---|---|
Format: | Artikel |
Sprache: | eng |
Schlagworte: | |
Online-Zugang: | Volltext bestellen |
Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
Zusammenfassung: | Astron. J. 166, 167 (2023) The bright star $\lambda$ Ser hosts a hot Neptune with a minimum mass of 13.6
$M_\oplus$ and a 15.5 day orbit. It also appears to be a solar analog, with a
mean rotation period of 25.8 days and surface differential rotation very
similar to the Sun. We aim to characterize the fundamental properties of this
system, and to constrain the evolutionary pathway that led to its present
configuration. We detect solar-like oscillations in time series photometry from
the Transiting Exoplanet Survey Satellite (TESS), and we derive precise
asteroseismic properties from detailed modeling. We obtain new
spectropolarimetric data, and we use them to reconstruct the large-scale
magnetic field morphology. We reanalyze the complete time series of
chromospheric activity measurements from the Mount Wilson Observatory, and we
present new X-ray and ultraviolet observations from the Chandra and Hubble
space telescopes. Finally, we use the updated observational constraints to
assess the rotational history of the star and to estimate the wind braking
torque. We conclude that the remaining uncertainty on stellar age currently
prevents an unambiguous interpretation of the properties of $\lambda$ Ser, and
that the rate of angular momentum loss appears to be higher than for other
stars with similar Rossby number. Future asteroseismic observations may help to
improve the precision of the stellar age. |
---|---|
DOI: | 10.48550/arxiv.2308.09808 |