Stratification with Optical Depth of the 5 Minute Oscillation through the Solar Photosphere

Cobo, B. Ruiz; Hidalgo, Inés Rodríguez; Collados, M.

doi:10.1086/304688

Cited by 17 publications

(13 citation statements)

References 28 publications

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“…However, the intensity amplitude behaviour is somewhat different: in particular, we do not observe its amplification with height. Our velocity amplitudes and phase shifts are also consistent with the results of Ruiz Cobo et al (1997) who applied the inversion techniques method to extract oscillatory properties. The magnitude of the temperature variations given by these authors agrees with the output of the theory of wave propagation we have applied, but its run with height is different.…”

Section: Height Dependence Of the Amplitudes And Phasessupporting

confidence: 88%

“…The magnitude of the temperature variations given by these authors agrees with the output of the theory of wave propagation we have applied, but its run with height is different. As was pointed out by Ruiz Cobo et al (1997), the interpretation of the temperature variations following from the inversion is not straightforward because they may be influenced by the variations in the opacity. However, amplitudes of temperature variations calculated by us for the 1D model MACKKL (Maltby et al 1986) are very similar to those given in Bertello & Caccin (1990).…”

Section: Height Dependence Of the Amplitudes And Phasesmentioning

confidence: 98%

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Five-minute oscillations above granules and intergranular lanes

Khomenko

Костик

Shchukina

2001

A&A

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Abstract. We discuss the links between the photospheric 5-min oscillations and the granulation pattern using a 30-min time series of CCD spectrograms of solar granulation recorded with high spatial (0 5) and temporal (9.3 s) resolution. The observed images contain the Fe i 5324Å spectral line with good height coverage from the low photosphere up to the temperature minimum region. Amplitudes, phases and periods of the 5-min oscillations are found to be different above granules and intergranular lanes. Strong oscillations occur well separated temporally and spatially. Many features of this different behaviour can be described in the frame of a relatively simple model of wave propagation in the solar atmosphere. To that aim, we have introduced oscillations into a 3D snapshot of a theoretical time dependent solar model atmosphere. NLTE synthesis of the time series of the Fe i 5324Å line profiles was performed taking into account granular and oscillatory components of the velocity field. Both, observations and theoretical modeling, lead to similar results: (i) oscillations above granules and intergranular lanes occur with different periods; (ii) the most energetic intensity oscillations occur above intergranular lanes; the most energetic velocity oscillations occur above granules and lanes with maximum contrast, i.e. above the regions with maximum convective velocities; (iii) velocity oscillations at the lower layers of the atmosphere lead oscillations at the upper layers in intergranular lanes. In granules the phase shift is nearly zero. We conclude that differences in oscillations above granules and lanes are caused mainly by variations of the physical conditions in these structures.

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Section: Height Dependence Of the Amplitudes And Phasessupporting

confidence: 88%

Section: Height Dependence Of the Amplitudes And Phasesmentioning

confidence: 98%

Five-minute oscillations above granules and intergranular lanes

Khomenko

Костик

Shchukina

2001

A&A

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“…The line-depth data also gives the information about the temperature variation but in the intermediate photospheric region (between Doppler velocity and continuum intensity) where the waves may no longer be purely isothermal (or adiabatic). One has to be careful with this interpretation because of the opacity variations induced by the temperature variation (see for example, Ruiz Cobo et al 1997). The line-depth measurements are also liable to contamination from Doppler motion of the spectral line.…”

Section: Discussionmentioning

confidence: 99%

Solar $\vec{p}$-modes and surface magnetic fields: Is there an acoustic emission?

Jain¹,

Haber²

2002

A&A

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Abstract.We study the effect of magnetism on the surface amplitude of p-modes by creating power maps using Doppler velocity, line-depth and continuum intensity data taken by the Michelson Doppler Interferometer (MDI) instrument on board SOHO. This analysis, using proper tracking procedures, of MDI line-depth data and its comparison with the simultaneous Doppler velocity data is the first such analysis. All three datasets show that the p-mode power is suppressed in the magnetic region with suppression increasing with field strength. However, in the high-frequency range, the power is enhanced in the Doppler velocity and line-depth data but not in continuum intensity. This enhancement, when present, appears to be in intermediate field strength elements in the immediate vicinity of a magnetically active region.

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“…In the past years they have become extensively used for the inversion of line profiles and Stokes spectra (Ruiz Cobo & del Toro Iniesta 1992;Bellot Rubio et al 1997). By means of RF s one can estimate the heights of formation for measurements that are obtained from observed quantities (Sánchez Almeida et al 1996).…”

Section: Calculation Of Response Functionsmentioning

confidence: 99%

Investigation of temperature and velocity fluctuations through the solar photosphere with the Na I D lines

Eibe¹,

Mein²,

Roudier³

et al. 2001

A&A

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Abstract. In this work we explore the diagnostic properties of the Na I D resonance lines by calculating the response functions of their line profiles to temperature and velocity perturbations in the atmosphere. We propose a method to transform spectral line intensity fluctuations measured at several wavelengths into temperature and velocity disturbances at different height levels. Results from tests done with several theoretical models of perturbations are discussed. Perturbations that vary as linear functions of depth are efficiently reproduced. The method also provides good estimations for exponential models. As an example we present an application to solar granulation data obtained with Multichannel Subtractive Double Pass (MSDP) spectroscopy.

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Stratification with Optical Depth of the 5 Minute Oscillation through the Solar Photosphere

Cited by 17 publications

References 28 publications

Five-minute oscillations above granules and intergranular lanes

Five-minute oscillations above granules and intergranular lanes

Solar $\vec{p}$-modes and surface magnetic fields: Is there an acoustic emission?

Investigation of temperature and velocity fluctuations through the solar photosphere with the Na I D lines

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