ADIPLS—the Aarhus adiabatic oscillation package

By J. Christensen-Dalsgaard. 2007

326 citations recorded by the source corpus.

Abstract Development of the Aarhus adiabatic pulsation code started around 1978. Although the main features have been stable for more than a decade, development of the code is continuing, concerning numerical properties and output. The code has been provided as a generally available package and has seen substantial use at a number of installations. Further development of the package, including bringing the documentation closer to being up to date, is planned as part of the HELAS Coordination Action.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Ocean Engineering

View Paper: https://www.semanticscholar.org/paper/1220ce76a0016edccbdb1b3f85c241d703b4fa78

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. D. Stello
3. Aaron Dotter
4. W. Chaplin
5. T. Bedding
6. A. Miglio
7. B. Paxton
8. B. Mosser

In Atomic and Molecular Physics, and Optics

1. B. Paxton
2. Matteo Cantiello
3. Aaron Dotter
4. W. Ball
5. L. Bildsten
6. Laurent Gizon
7. A. Miglio
8. D. Stello

In Ocean Engineering

1. W. Ball
2. Laurent Gizon
3. Matteo Cantiello
4. A. Miglio
5. B. Paxton
6. D. Stello
7. P. Eggenberger
8. L. Bildsten

Citations in the corpus

• AN ANCIENT EXTRASOLAR SYSTEM WITH FIVE SUB-EARTH-SIZE PLANETS (2015, methodology): “…relies on a dense grid of stellar models computed with the GARching STellar Evolution Code (GARSTEC; Weiss & Schlattl 2008) including the effects of microscopic diffusion, and on theoretical frequencies calculated using the Aarhus aDIabatic PuLSation code (ADIPLS; Christensen-Dalsgaard 2008a).”
• CALCULATING ASTEROSEISMIC DIAGRAMS FOR SOLAR-LIKE OSCILLATIONS (2011, methodology): “A grid of 51000 stellar models was calculated from the ZAMS to almost the tip of the red-giant branch using ASTEC (Christensen-Dalsgaard 2008a) with the EFF equation of state (Eggleton et al. 1973).”
• A UNIFORM ASTEROSEISMIC ANALYSIS OF 22 SOLAR-TYPE STARS OBSERVED BY KEPLER (2012, methodology): “The oscillation properties of the models are derived by computing the individual frequencies with the Aarhus adiabatic pulsation code (ADIPLS; Christensen-Dalsgaard 2008b).”
• Determining global parameters of the oscillations of solar-like stars (2009, methodology): “We use the Aarhus Stellar Evolution Code (ASTEC) coupled to an adiabatic pulsation code (ADIPLS) (Christensen-Dalsgaard 2008b,a).”
• ANGULAR MOMENTUM TRANSPORT WITHIN EVOLVED LOW-MASS STARS (2014, methodology): “The MESA background structure and rotational profiles are then used in ADIPLS to calculate the splitting of mixed modes for different angular momentum transport mechanisms.”
• Angular momentum transport in stellar interiors constrained by rotational splittings of mixed modes in red giants (2012, methodology): “The rotational splittings of the dipole modes ( = 1) are then computed for this model using the Aarhus adiabatic pulsation code (Christensen-Dalsgaard 2008).”
• Modules for Experiments in Stellar Astrophysics (MESA): Time-dependent Convection, Energy Conservation, Automatic Differentiation, and Infrastructure (2022, methodology): “Atmosphere Reconstruction for Pulsation Codes As discussed in MESA II and MESA III, MESA can pass models to the ADIPLS (Christensen-Dalsgaard 2008) or GYRE (Townsend & Teitler 2013) linear pulsation codes, either in-memory during an astero-module optimization or via files written to disk in a…”
• Seismic diagnostics for transport of angular momentum in stars. I. Rotational splittings from the pre-main sequence to the red-giant branch. (2012, methodology): “…we follow the evolution of theoretical linear rotational splittings for a .3 M⊙ sequence of stellar models evolved from the PMS to the RGB. Theℓ = 1, 2 modes are computed with the ADIPLS code (Christensen-Dalsgaard 2008) in a frequency range where th modes are expected to be stochastically excited.”
• A new correction of stellar oscillation frequencies for near-surface effects (2014, methodology): “Calls to ADIPLS are made from MESA during the stellar evolution calculation and by default return the frequencies and inertiae.”
• The Updated BaSTI Stellar Evolution Models and Isochrones. I. Solar-scaled Calculations (2018, methodology): “We have computed adiabatic oscillation frequencies for all the models using the Aarhus aDIabatic PuLSation package (ADIPLS, Christensen-Dalsgaard 2008).”
• MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA): PLANETS, OSCILLATIONS, ROTATION, AND MASSIVE STARS (2013, methodology): “It is a pleasure to thank Falk Herwig for significant contributions to the MESA project and Jørgen Christensen-Dalsgaard for kindly providing the ADIPLS code for inclusion in MESA and assisting with its integration.”
• Standing on the Shoulders of Dwarfs: the Kepler Asteroseismic LEGACY Sample. II. Radii, Masses, and Ages (2016, methodology): “ASTFIT The ”ASTEC FITting” method uses the ASTEC evolutionary code (Christensen-Dalsgaard 2008b) coupled to ADIPLS (Christensen-Dalsgaard 2008a) for computation of theoretical pulsation frequencies in a grid of stellar models.”
• Modules for Experiments in Stellar Astrophysics ( ): Convective Boundaries, Element Diffusion, and Massive Star Explosions (2017, background): “Examples include ADIPLS (Christensen-Dalsgaard 2008; Christensen-Dalsgaard & Thompson 2011), GYRE (Townsend & Teitler 2013), and STELLA (Blinnikov et al. 1998; Blinnikov & Sorokina 2004; Baklanov et al. 2005; Blinnikov et al. 2006).”
• Ages and fundamental properties of Kepler exoplanet host stars from asteroseismology (2015, methodology): “This allows direct comparison of theoretical frequencies with the observed quantities without resorting to a surface correction, such as the power-law term applied to a solar model to reproduce the helioseismic observations (e.g., Kjeldsen, Bedding & Christensen-Dalsgaard 2008).”
• MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA): BINARIES, PULSATIONS, AND EXPLOSIONS (2015, methodology): “…and NEWYUO (Powell 2004) algorithms for χ2 minimization; parameter optimization using only spectroscopic constraints (e.g., Teff and surface gravity); and coupling to the GYRE oscillation code, as an alternative to the ADIPLS code (Christensen-Dalsgaard 2008) used in the original implementation.”