The Inversion Problem

Gough, D. O.; Thompson, M. J.

doi:10.2307/j.ctt1zxsmjb.19

Cited by 47 publications

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“…This is a consequence of the linearity hypothesis used to compute the structural corrections from seismic observations. To obtain the corrections of integrated quantities, we use the linear relations between frequency and structure from [20] …”

Section: Inversion Proceduresmentioning

confidence: 99%

Asteroseismic inversions in the Kepler era: application to the Kepler Legacy sample

2017

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Abstract. In the past few years, the CoRoT and Kepler missions have carried out what is now called the space photometry revolution. This revolution is still ongoing thanks to K2 and will be continued by the Tess and Plato2.0 missions. However, the photometry revolution must also be followed by progress in stellar modelling, in order to lead to more precise and accurate determinations of fundamental stellar parameters such as masses, radii and ages. In this context, the long-lasting problems related to mixing processes in stellar interior is the main obstacle to further improvements of stellar modelling. In this contribution, we will apply structural asteroseismic inversion techniques to targets from the Kepler Legacy sample and analyse how these can help us constrain the fundamental parameters and mixing processes in these stars. Our approach is based on previous studies using the SOLA inversion technique [1] to determine integrated quantities such as the mean density [2], the acoustic radius, and core conditions indicators [3], and has already been successfully applied to the 16Cyg binary system [4]. We will show how this technique can be applied to the Kepler Legacy sample and how new indicators can help us to further constrain the chemical composition profiles of stars as well as provide stringent constraints on stellar ages.

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Section: Inversion Proceduresmentioning

confidence: 99%

Asteroseismic inversions in the Kepler era: application to the Kepler Legacy sample

2017

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“…Hence, by assuming that aspherical sound speed perturbations are negligible, with the internal rotational structure as inferred from the helioseismology (section 4.2), contribution due to second order rotational effects is computed and is subtracted from the even degree frequency splittings and, resulting residual of even degree splittings are compared with the computed frequency splittings due to assumed magnetic field structure. Detailed inversion procedures can be found in the previous studies Gough and Thompson 1991;Dziembowski and Goode 1991;Basu 1997;Antia, Chitre and Thompson 2000;Antia 2002;Baldner et. al.…”

Section: Inference Of Magnetic Field Structure : Primary Inversionsmentioning

confidence: 99%

Seismology of the Sun: Inference of Thermal, Dynamic and Magnetic Field Structures of the Interior

Hiremath

2013

New Trends in Atomic and Molecular Physics

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Recent overwhelming evidences show that the sun strongly influences the Earth's climate and environment. Moreover existence of life on this Earth mainly depends upon the sun's energy. Hence, understanding of physics of the sun, especially the thermal, dynamic and magnetic field structures of its interior, is very important. Recently, from the ground and space based observations, it is discovered that sun oscillates near 5 min periodicity in millions of modes. This discovery heralded a new era in solar physics and a separate branch called helioseismology or seismology of the sun has started. Before the advent of helioseismology, sun's thermal structure of the interior was understood from the evolutionary solution of stellar structure equations that mimicked the present age, mass and radius of the sun. Whereas solution of MHD equations yielded internal dynamics and magnetic field structure of the sun's interior. In this presentation, I review the thermal, dynamic and magnetic field structures of the sun's interior as inferred by the helioseismology.

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“…[6]) and the alternative methods used in inverting Duvall's law (Gough & Thompson 1991) can be implemented by replacing with and w with .…”

Section: ) Mpr/2gmentioning

confidence: 99%

“…This curve describes Duvall's law through an integral equation of the Abel type that connects the frequencies with the radial sound speed. The Abel equation can be analytically inverted in various ways to obtain the radial sound speed (Gough & Thompson 1991).…”

Section: Introductionmentioning

confidence: 99%

Equivalence between Duvall’s Law and the Time-Distance Curve

D'Silva

2001

The Astrophysical Journal

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Duvall's law is shown to be equivalent to the phase time-distance curve. The two are connected through a simple transformation. Thus, like Duvall's law, the phase time-distance curve can be analytically inverted to obtain the radial sound speed. The use of the phase information of the time-distance technique makes the inversion of the time-distance Duvall law particularly advantageous over the traditional inversion of Duvall's law. The radial sound speed can also be obtained numerically through the radial limit of the global or local tomography of the Sun. With global tomography, one can take advantage of the higher order skips of wave packets to obtain local tomograms of any section of the Sun, including the interior of the farside, that currently cannot be directly observed.

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The Inversion Problem

Cited by 47 publications

References 0 publications

Asteroseismic inversions in the Kepler era: application to the Kepler Legacy sample

Asteroseismic inversions in the Kepler era: application to the Kepler Legacy sample

Seismology of the Sun: Inference of Thermal, Dynamic and Magnetic Field Structures of the Interior

Equivalence between Duvall’s Law and the Time-Distance Curve

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