By Regina von Berlepsch
This twenty second quantity within the sequence comprises 15 invited experiences and spotlight contributions from remarkable audio system provided through the 2009 annual assembly of the Astronomical Society with reference to "Deciphering the Universe via Spectroscopy", held in Potsdam, Germany.Topics diversity from the measurements of magnetic fields at the floor of the solar through precise measurements of abundances in stellar atmospheres to the kinematics of the universe at its biggest scales. the result's a scientific evaluation of the newest astronomical and cosmological learn.
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Extra info for Reviews in Modern Astronomy, Deciphering the Universe through Spectroscopy (Volume 22)
2010c) exist for HS 2231+2441 and NSVS 14256825. A different type of detection has been put forward by Geier et al. 4 d orbit. Based on the above and this ﬁnding (that yet has to be conﬁrmed), these authors also argue for a decisive inﬂuence of sub-stellar companions on the late stages of stellar evolution. The EXOTIME program aims to increase the empirical data available on which to base such discussions. 1 The planet-hosting pulsating sdB V391 Pegasi V391 Pegasi (HS 2201+2610) was ﬁrst discovered to be a rapidly pulsating subdwarf B star by Østensen et al.
The value for vrot is in principle accessible through rotational splitting in the photometric frequency spectrum (which has however not been found for V391 Pegasi yet), while the projected rotational velocity vrot sin i can be measured from the rotational broadening of spectral lines. This rotational broadening must be deconvolved from the additional pulsational broadening caused by the surface radial velocity variation in high S/N phase averaged spectra. Both phase averaged and phase resolved high resolution échelle spectra were obtained in May and September 2007 with the Hobby-Eberly Telescope (HET), and one phase averaged spectrum in May 2008 with the Keck 1 telescope, in order to Pulsations and planets: The asteroseismology-extrasolar-planet connection 41 Figure 3: Detail of the observed Hα core in a pulsation-integrated Keck spectrum of V391 Pegasi.
The equilibrium is restored by the actions of pressure and buoyancy, with one of the two usually dominating in a particular region of the star. , if the mode geometry yields a detectable net effect in the integrated observables). Given appropriate modelling capabilities, the density structure of a star can be inferred from observations of a sufﬁciently large number of excited eigenmodes that probe the interior conditions differentially. While the exact analysis approach can vary depending on the class of variables considered, important fundamental parameters that can be derived from this exercise are the stellar mass, radius and (depthdependent) chemical composition.