Porto Oscillation Code (posc)

Monteiro, M. J. P. F. G.

doi:10.1007/s10509-008-9802-y

Cited by 12 publications

(9 citation statements)

References 11 publications

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“…A key tool in this development will be the application of the techniques to artificial data; such tests were carried out before the launch of the missions (e.g., Monteiro et al 2002;Mazumdar 2005) but have since largely been ignored in the flush of real data. Similarly, further work is needed to understand the differences between results of different stellar evolution and pulsation codes, as started in the ESTA project in preparation for the CoRoT mission (Monteiro 2008). Finally, it is probably time to consider the application of the inverse techniques discussed in Sect.…”

Section: Discussionmentioning

confidence: 99%

Stellar model fits and inversions

Christensen‐Dalsgaard

2012

Astron Nachr

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The recent asteroseismic data from the CoRoT and Kepler missions have provided an entirely new basis for investigating stellar properties. This has led to a rapid development in techniques for analysing such data, although it is probably fair to say that we are still far from having the tools required for the full use of the potential of the observations. Here I provide a brief overview of some of the issues related to the interpretation of asteroseismic data.

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Section: Discussionmentioning

confidence: 99%

Stellar model fits and inversions

Christensen‐Dalsgaard

2012

Astron Nachr

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“…Various codes have been developed, such as ADIPLS, LOSC, PULSE, POSC, GraCo, NOSC, OSCROX, FILOU, LNAWNR, or GYRE (e.g. Christensen-Dalsgaard 2008a;Scuflaire et al 2008;Brassard and Charpinet 2008;Monteiro 2008;Moya and Garrido 2008;Provost 2008;Roxburgh 2008;Suárez and Goupil 2008;Suran 2008;Townsend and Teitler 2013). However, to understand the nature of the oscillations, we make some approximations.…”

Section: Acoustic Gravity and Mixed Modesmentioning

confidence: 99%

Asteroseismology of solar-type stars

García

Ballot

2019

Living Rev Sol Phys

155

100

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Until the last few decades, investigations of stellar interiors had been restricted to theoretical studies only constrained by observations of their global properties and external characteristics. However, in the last 30 years the field has been revolutionized by the ability to perform seismic investigations of stellar interiors. This revolution begun with the Sun, where helioseismology has been yielding information competing with what can be inferred about the Earth’s interior from geoseismology. The last two decades have witnessed the advent of asteroseismology of solar-like stars, thanks to a dramatic development of new observing facilities providing the first reliable results on the interiors of distant stars. The coming years will see a huge development in this field. In this review we focus on solar-type stars, i.e., cool main-sequence stars where oscillations are stochastically excited by surface convection. After a short introduction and a historical overview of the discipline, we review the observational techniques generally used, and we describe the theory behind stellar oscillations in cool main-sequence stars. We continue with a complete description of the normal mode analyses through which it is possible to extract the physical information about the structure and dynamics of the stars. We then summarize the lessons that we have learned and discuss unsolved issues and questions that are still unanswered.

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“…Using the POSC code (Monteiro 2008), linear adiabatic frequencies were calculated for each model, for modes with = 0, 1, and 2. The large separations, defined as the difference between the frequencies of consecutive modes of the same degree , were also computed.…”

Section: Resultsmentioning

confidence: 99%

On the possibility of using seismic probes to study the core composition in pulsating white dwarfs

Faria¹,

Monteiro²

2012

Astron Nachr

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White dwarfs correspond to the final stages of stellar evolution of solar-type stars. In these objects, production of energy by nuclear burning has ended which means that a white dwarf simply cools down over the course of the next billion years. It is now known that white dwarfs spend some of their cooling history in an instability strip. The pulsating white dwarfs with an hydrogen atmosphere (called DAV or ZZ Ceti stars) show non-radial oscillation modes with periods in the range 100-1200 s. In this work we try to illustrate how the oscillation p-mode frequencies of idealized white dwarf models change as the result of a different chemical composition in the core, with the ultimate goal of determining the chemical stratification from seismic observations. The presence of acoustic glitches in the internal structure results in a periodic signal in the frequencies. We find that this signal depends on the chemical stratification/composition of the core in a form that can be analytically modelled.

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Porto Oscillation Code (posc)

Cited by 12 publications

References 11 publications

Stellar model fits and inversions

Stellar model fits and inversions

Asteroseismology of solar-type stars

On the possibility of using seismic probes to study the core composition in pulsating white dwarfs

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