Determining the Inclination of the Rotation Axis of a Sun-like Star

By Laurent Gizon, S. Solanki. 2003

234 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/183ed809580f9ed219d90b0174e0369608aef68e

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

1. D. Huber
2. W. Chaplin
3. D. Stello
4. A. Miglio
5. T. Bedding
6. B. Mosser
7. J. Winn
8. S. Hekker

In Instrumentation

1. W. Chaplin
2. D. Huber
3. D. Stello
4. B. Mosser
5. T. Bedding
6. A. Miglio
7. S. Hekker
8. J. Winn

In Statistical and Nonlinear Physics

1. K. Schlaufman
2. D. Huber
3. J. Winn
4. W. Chaplin
5. A. Miglio
6. S. Basu
7. Y. Elsworth
8. D. Fabrycky

Citations in the corpus

• EXOPLANETARY SPIN–ORBIT ALIGNMENT: RESULTS FROM THE ENSEMBLE OF ROSSITER–MCLAUGHLIN OBSERVATIONS (2009, background): “Usually there is no direct measurement of is, although it is possible to constrain is via asteroseismology (Gizon & Solanki 2003) or by combining estimates of the stellar radius, stellar rotation period, and projected rotational velocity (see, e.g., Winn et al. 2007a).”
• Standing on the Shoulders of Dwarfs: the Kepler Asteroseismic LEGACY Sample. I. Oscillation Mode Parameters (2016, background): “(see, Dziembowski 1977; Gizon & Solanki 2003); Ṽ2l denotes the squared visibility (power units) of a non-radial mode relative to a radial mode at the same frequency, i.e., Ṽ2l = (Vl/V0) 2 and Ṽ2tot = ∑ l Ṽ2l , (3.2) from the spatial filtering resulting from integrating the intensity for a mode…”
• CoRoT sounds the stars: p-mode parameters of Sun-like oscillations on HD 49933 (2008, methodology): “However, the inclination can in principle be constrained by asteroseismology, provided the mode amplitude ratios can be measured reliably (Gizon & Solanki 2003).”
• Asteroseismology of red giants from the first four months of Kepler data: Fundamental stellar parameters (2010, background): “…for this we have included rotationally split components for thel = 1 and 2 modes, which are parameterised by a single rotational frequency and an inclination angle that defines the height ratio between the central profile and the split components (e.g., Gizon & Solanki 2003; Ballot et al. 2006).”
• Determining global parameters of the oscillations of solar-like stars (2009, methodology): “Thanks to seismology, we can independently determine the inclination from the relative amplitude of mode components inside multiplets (Gizon & Solanki 2003).”
• The Occurrence and Architecture of Exoplanetary Systems (2014, background): “Crucially, the relative visibilities of the modes within each multiplet depend on viewing angle; the observed amplitudes thereby divulge the stellar obliquity (Gizon & Solanki 2003).”
• The Rossiter-McLaughlin Effect and Analytic Radial Velocity Curves for Transiting Extrasolar Planetary Systems (2004, unknown): “Furthermore, the combined data analysis with asteroseismology (e.g., Gizon & Solanki 2003) and/or the correlation between the mean level of emission and the rotation period (e.g., Noyes et al. 1984) may break the degeneracy between V and Is in extrasolar planetary systems.”
• Asteroseismology of Solar-Type and Red-Giant Stars (2013, methodology): “…oscillators, measurement of the observed relative power of the different azimuthal components in each non-radial mode provides a direct estimate of i (for a detailed discussion of the method, see Gizon & Solanki 2003, Ballot, Garćıa & Lambert 2006, Ballot et al. 2008, Chaplin et al. 2013).”
• ASTEROSEISMIC CLASSIFICATION OF STELLAR POPULATIONS AMONG 13,000 RED GIANTS OBSERVED BY KEPLER (2013, background): “We see two peaks when the inclination is high (close to 90 degrees), three peaks are seen when the inclination is intermediate (∼40–60 degrees), and just one peak is seen when the star is viewed pole on (Gizon & Solanki 2003).”
• SEISMIC EVIDENCE FOR A RAPIDLY ROTATING CORE IN A LOWER-GIANT-BRANCH STAR OBSERVED WITH KEPLER (2012, background): “Inside a rotational multiplet, the height ratios only depend on the inclination angle i of the star (Gizon & Solanki 2003) and correspond to the terms al,m(i) in Eq.”
• EVIDENCE OF POSSIBLE SPIN–ORBIT MISALIGNMENT ALONG THE LINE OF SIGHT IN TRANSITING EXOPLANET SYSTEMS (2010, background): “Astrosiesmology measurements of is are also possible in special circumstances (Gizon & Solanki 2003).”
• Determining stellar macroturbulence using asteroseismic rotational velocities from Kepler (2014, methodology): “…disc depend only on the angular distance from the disc centre, as is the case for photometric observations, and there is energy equipartition between the different m components, as is the case for the modest rates of rotation considered here, we may use the formulation of Gizon & Solanki (2003).”