The Star Formation History of Nearby Dwarf Galaxies: problems, methods and results
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Aparicio, Antonio
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1998
This section contains the publications database that collects IAC articles published in scientific journals. Please, click on the arrow to see full search filter and sort options: author, journal, year, etc..
It also provides access to IAC Preprints Repository here: https://research.iac.es/preprints/
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The star formation history of Leo INot AvailableGallart, Carme et al.
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The Solar Acoustic Spectrum as Seen by GOLF. IV. Linewidth, Power and Energy of the ModesThe model fitted to the observed spectra also allows the measurement of the linewidth and power of each mode (see poster II). The linewidths are related to the damping mechanisms and the energies give information on the excitation mechanisms. Here the results of these parameters as well as the relative energy shared by the components of a givenRoca-Cortés, T. et al.
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The Solar Acoustic Spectrum as Seen by GOLF. III. Asymmetries, Resonant Frequencies and SplittingsThe definition of the model to fit to the observed spectra depends on the physics we are assuming is present in the phenomena we are observing. Here we present the results obtained following the fit of several models (described in poster II). Therefore the effects of asymmetrical line shapes, a common background for all modes, fixed relative powerRoca-Cortés, T. et al.
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The Solar Acoustic Spectrum as Seen by GOLF. II. Noise Statistics Background and Methods of AnalysisData acquired by GOLF experiment onboard SOHO during ~20 months has been analysed. GOLF is a disk-integrated sunlight experiment therefore biased to observe very low ell modes (ell 3). However the excellent ratio signal to background (S/B) achieved permits also the detection of some modes with 4 ell 6 and those from n >= 8 up to the cut-offRoca-Cortés, T. et al.
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The Solar Acoustic Spectrum as Seen by GOLF. I. The Difficult Case: Modes With n<10Below 1.3 mHz the solar background level increases as well as the energy of the solar acoustic modes decreases. This situation yields the detection of low degree p-modes extremely difficult because the signal to background ratio is very small (S/B ll 1). Yet, these modes are of paramount importance to be able to infer the structure of the solarRégulo, C. et al.
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