Why does the pulsation frequency in a roAp star increase with a stronger magnetic field, without changing the frequency interval?
#Astrophysics #Stars #Asteroseismology #Spectroscopy

New in the #VirtualObservatory: “Characterizing bright delta Scuti pulsators” by Mani P. et al.
https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/552/G1780
#VariableStars #Asteroseismology #VisibleAstronomy

There is a hypothesis that the magnetic field strength in Przybylski's Star decreases at a rate of about 18 G per year.
But this may be due to insufficient measurements... sounds like an interesting question to get into!
#Astrophysics #Stars #Asteroseismology #Spectroscopy

7/ Source: Mkrtichian et al., "The detection of the rich p-mode spectrum and asteroseismology of Przybylski's star."
#Astrophysics #Stars #Asteroseismology #Spectroscopy

Another way to measure stellar parameters is to compare predicted and observed pulsations.
But how can we tell whether the frequency we observe is a single oscillation mode, and not a mixture of several unresolved modes?
#Astrophysics #Stars #Asteroseismology #Spectroscopy

The pulsation phase in Przybylski's Star does not change by more than 0.15 of a period for most spectral lines.
#Astrophysics #Stars #Asteroseismology #Spectroscopy

#Astrophysics #Stars #Spectroscopy #Asteroseismology

6/ Source: Mkrtichian et al., "The detection of the rich p-mode spectrum and asteroseismology of Przybylski's star."
#Astrophysics #Stars #Asteroseismology #ChemicallyPeculiarStars

How can p-mode pulsations in Przybylski's Star be produced at many different frequencies? What is the mechanism?
#Astrophysics #Stars #Asteroseismology #ChemicallyPeculiarStars

New in the #VirtualObservatory: “Solar-like oscillations using TESS 2” by Feng Y. et al.
https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/283/12
#ChemicalAbundances #EffectiveTemperature #Asteroseismology #VariableStars