Physics of solar-like oscillations

By J. Christensen-Dalsgaard. 2004

147 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/29b59f10b72dc85cbaaaf3b4ea8d27a3d7d17fee

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

AN ANCIENT EXTRASOLAR SYSTEM WITH FIVE SUB-EARTH-SIZE PLANETS (2015, background): “These so-called p modes – with the pressure gradient playing the role of the restoring force – are characterized by being intrinsically damped while simultaneously stochastically excited by near-surface convection (Christensen-Dalsgaard 2004).”
Planetary detection limits taking into account stellar noise - I. Observational strategies to reduce stellar oscillation and granulation effects (2010, background): “Theory predicts that frequencies of p-modes riseup with the square root of the star mean density and that their amplitudes are proportional to the luminosity over mass ratio (Christensen-Dalsgaard 2004).”
FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM KEPLER AND CoRoT AND INTERFEROMETRY FROM THE CHARA ARRAY (2012, methodology): “Asteroseismology, the study of stellar oscillations, is a powerful method to determine properties of solar-type stars such as the mean stellar density with little model dependence (see, e.g., Brown & Gilliland 1994; Christensen-Dalsgaard 2004; Aerts et al. 2010).”
TESTING SCALING RELATIONS FOR SOLAR-LIKE OSCILLATIONS FROM THE MAIN SEQUENCE TO RED GIANTS USING KEPLER DATA (2011, methodology): “One of the most powerful methods to constrain fundamental properties of field stars is asteroseismology (see, e.g., Brown & Gilliland 1994; Christensen-Dalsgaard 2004; Aerts et al. 2010).”
SOLAR-LIKE OSCILLATIONS IN LOW-LUMINOSITY RED GIANTS: FIRST RESULTS FROM KEPLER (2010, background): “The large peak height can be explained by the fact that mixed modes are expected to have longer lifetimes (smaller linewidths) than pure p modes because they have larger mode inertias (e.g., Christensen-Dalsgaard 2004).”
Mixed modes in red-giant stars observed with CoRoT (2011, methodology): “The theoretical analysis of these mixed modes in red giants has been performed prior to observations (Dziembowski et al. 2001; Christensen-Dalsgaard 2004; Dupret et al. 2009).”
HAT-P-11b: A SUPER-NEPTUNE PLANET TRANSITING A BRIGHT K STAR IN THE KEPLER FIELD (2009, background): “The “large splitting” of p-mode frequencies yields direct information on the radius of the star, and their “small splitting” gives information on the H/He ratio in the core and hence the age of the star (e.g. Christensen-Dalsgaard 2004).”
ASTEROSEISMOLOGY OF RED GIANTS FROM THE FIRST FOUR MONTHS OF KEPLER DATA: GLOBAL OSCILLATION PARAMETERS FOR 800 STARS (2010, background): “Stars with convective envelopes show solar-like oscillations that are sensitive to the physical processes governing their interiors (see, e.g., Brown & Gilliland 1994; Christensen-Dalsgaard 2004).”
Asteroseismology of red giants from the first four months of Kepler data: Fundamental stellar parameters (2010, background): “Studying solar-type oscillations has proved to be a powerful way to test the physical processes in stars (e.g. Christensen-Dalsgaard 2004) that are similar to our Sun and also to the more evolved red giants, which represent the future of our Sun.”
CALCULATING ASTEROSEISMIC DIAGRAMS FOR SOLAR-LIKE OSCILLATIONS (2011, background): “Theoretical studies of red giants predict a very dense frequency spectrum of non-radial modes (Dziembowski et al. 2001; Christensen-Dalsgaard 2004; Dupret et al. 2009; Montalbán et al. 2010; Di Mauro et al. 2011; Christensen-Dalsgaard 2011).”
Probing the core structure and evolution of red giants using gravity-dominated mixed modes observed with Kepler (2012, background): “Mixed modes, theoretically described in previous work25 (e.g. Dziembowski et al. 2001; Christensen-Dalsgaard 2004; Dupret et al. 2009, and references therein), were reported in red giants by Bedding et al. (2010), who attributed the broadening of the ℓ = 1 ridge to the presence of multiple ℓ = 1…”