Synthetic spectral analysis of a kinetic model for slow-magnetosonic waves in solar corona

Journal Article · Fri Mar 25 04:00:00 EDT 2016 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.4943805· OSTI ID:22590897

Ruan, Wenzhi; He, Jiansen; Tu, Chuanyi; Wang, Linghua ^[1]; Zhang, Lei ^[2]; Vocks, Christian ^[3]; Marsch, Eckart ^[4]; Peter, Hardi ^[5]

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1. School of Earth and Space Sciences, Peking University, Beijing, 100871, China, E-mail: [e-mail] (China)
2. State Key Laboratory of Space Weather, Chinese Academy of Sciences, Beijing 100190 (China)
3. Leibniz-Institut für Astrophysik Potsdam, 14482, Potsdam (Germany)
4. Institute for Experimental and Applied Physics, Christian-Albrechts-Universität zu Kiel, 24118 Kiel (Germany)
5. Max Plank Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen (Germany)

We propose a kinetic model of slow-magnetosonic waves to explain various observational features associated with the propagating intensity disturbances (PIDs) occurring in the solar corona. The characteristics of slow mode waves, e.g, inphase oscillations of density, velocity, and thermal speed, are reproduced in this kinetic model. Moreover, the red-blue (R-B) asymmetry of the velocity distribution as self-consistently generated in the model is found to be contributed from the beam component, as a result of the competition between Landau resonance and Coulomb collisions. Furthermore, we synthesize the spectral lines and make the spectral analysis, based on the kinetic simulation data of the flux tube plasmas and the hypothesis of the surrounding background plasmas. It is found that the fluctuations of parameters of the synthetic spectral lines are basically consistent with the observations: (1) the line intensity, Doppler shift, and line width are fluctuating in phase; (2) the R-B asymmetry usually oscillate out of phase with the former three parameters; (3) the blueward asymmetry is more evident than the redward asymmetry in the R-B fluctuations. The oscillations of line parameters become weakened for the case with denser surrounding background plasmas. Similar to the observations, there is no doubled-frequency oscillation of the line width for the case with flux-tube plasmas flowing bulkly upward among the static background plasmas. Therefore, we suggest that the “wave + beam flow” kinetic model may be a viable interpretation for the PIDs observed in the solar corona.

• OSTI ID: 22590897
• Journal Information: AIP Conference Proceedings, Journal Name: AIP Conference Proceedings Journal Issue: 1 Vol. 1720; ISSN APCPCS; ISSN 0094-243X
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ASTROPHYSICS
ASYMMETRY
COMPUTERIZED SIMULATION
DISTURBANCES
DOPPLER EFFECT
FLUCTUATIONS
LANDAU DAMPING
LINE WIDTHS
MAGNETOACOUSTIC WAVES
OSCILLATIONS
PLASMA
SOLAR ACTIVITY
SOLAR CORONA
VELOCITY