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B. N. Dwivedi

Publications and source records attributed to B. N. Dwivedi.

43 records · Page 3Linked to original sources
arXiv2008

Intensity oscillations observed with Hinode near the south pole of the Sun: leakage of low frequency magneto-acoustic waves into the solar corona

Aims. To study intensity oscillations in the solar chromosphere/corona above a quiet-Sun magnetic network. Methods. We analyse the time series of He II 256.32, Fe XI 188.23 and Fe XII 195.12 spectral lines observed by EUV Imaging Spectrometer (EIS) on board Hinode near the south pole. Then we use a standard wavelet tool to produce power spectra of intensity oscillations above the magnetic network. Results. We get ~7 min intensity oscillations in all spectral lines and ~13 min intensity oscillations only in He II with the probability of ~96-98 %, which probably reflects the process of magneto-acoustic wave propagation above the network. Conclusions. We suggest that field-free cavity areas under bipolar magnetic canopies in the vicinity of magnetic network may serve as resonators for the magneto-acoustic waves. The cavities with photospheric sound speed and granular dimensions may produce the waves with the observed periods. The waves may propagate upwards in the transition region/corona and cause observed intensity oscillations.

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arXiv2007

Long period slow MHD waves in the solar wind source region

We consider compressive viscosity and thermal conductivity to study the propagation and dissipation of long period slow longitudinal MHD waves in polar coronal holes. We discuss their likely role in the line profile narrowing, and in the energy budget for coronal holes and the solar wind. We compare the contribution of longitudinal MHD waves with high frequency Alfven waves.

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arXiv2007

Effect of the steady flow on spatial damping of small-amplitude prominence oscillations

Aims. Taking account of steady flow in solar prominences, we study its effects on spatial damping of small-amplitude non-adiabatic magnetoacoustic waves in a homogeneous, isothermal, and unbounded prominence plasma. Methods. We model the typical feature of observed damped oscillatory motion in prominences, removing the adiabaticity assumption through thermal conduction, radiation and heating. Invoking steady flow in MHD equations, we linearise them under small-amplitude approximation and obtain a new general dispersion relation for linear non-adiabatic magnetoacoustic waves in prominences Results. The presence of steady flow breaks the symmetry of forward and backward propagating MHD wave modes in prominences. The steady flow has dramatic influence on the propagation and damping of magnetoacoustic and thermal waves. Depending upon the direction and strength of flow the magnetoacoustic and thermal modes can show both the features of wave amplification and damping. At the wave period of 5 min where the photospheric power is maximum, the slow mode shows wave amplification. However, in the absence of steady flow the slow mode wave shows damping. Conclusions. For the wave period between 5 min and 15 min, the amplification length for slow mode, in the case of prominence regime 1.1, varies between 3.4*10^11 m to 2*10^12 m. Dramatic influence of steady flow on small-amplitude prominence oscillations is likely to play an important role in both wave detection and prominence seismology.

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arXiv2007

Dispersion Relation for MHD Waves in Homogeneous Plasma

We consider viscosity and thermal conductivity as dissipation mechanisms to derive a general dispersion relation for MHD waves propagating in a homogeneous plasma. We show that the actual dispersion relation for MHD waves in a homogeneous medium must be six-order. The finding is in agreement (except some coefficients) with the results of Porter et al. (1994) but it is in disagreement with the previous results obtained by Kumar et al. (2006). We also discuss in detail differences between our approach and those considered by other authors. Accepted, BASI

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arXiv2007

Comments on Viscous Damping of Non-Adiabatic MHD Waves in an Unbounded Solar Coronal Plasma by Kumar and Kumar

Considering thermal conduction, compressive viscosity and optically thin radiation as damping mechanisms for MHD waves, we derive a six-order general dispersion relation. We point out a fundamental flaw in the derivation of five-order dispersion relation by Kumar and Kumar (2006) who adopt as a basis vector. The correct definition of the motion in the x-z plane (2-D vector space) stems from the two independent variables, namely .

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arXiv2006

Significant Results from SUMER/SOHO

We briefly outline recent observations by solar spacecraft such as Yohkoh, SOHO, TRACE, and RHESSI, which have revolutionized what we know and don't know about the Sun. We then present some significant results, mainly from SUMER/SOHO but also complimentary from the other SOHO's experiments, such as CDS, EIT, UVCS, and LASCO. In particular, we present density-temperature structures, explosive events, velocity anisotropy, wave activity, coronal holes and the solar wind etc. These results have provided valuable clues to a better understanding of the two of the SOHO's principal scientific objectives namely, how the Sun's magnetic energy heats its million-degree corona, and feeds the solar wind.

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