Parametric generation of magnetoacoustic-gravity waves in the solar atmosphere

Petukhov, M. Yu.; Petukhov, Yu. V.

doi:10.1134/1.1544534

Cited by 1 publication

(2 citation statements)

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“…The propagation of MAWs in the solar atmosphere is affected by cutoff periods for these waves. Among different attempts to determine the cutoff for MAWs in the isothermal solar atmosphere with the uniform horizontal and vertical magnetic fields (e.g., Thomas 1983;Campos 1986;Musielak 1990;Stark & Musielak 1993;Petukhov & Petukhov 2003;Roberts 2006), we select the local cutoff period for MAWs obtained by Stark & Musielak (1993), which is given by…”

Section: Cutoff Frequencies For Magnetoacoustic Wavesmentioning

confidence: 99%

“…To make a distinction between propagating and standing waves, the concept of critical frequency was introduced; the critical frequency is a local quantity resembling a cutoff frequency. Further exploration of the critical and cutoff frequencies was done by Musielak (1990), Musielak et al (1992), Stark & Musielak (1993), and in more recent work by Petukhov & Petukhov (2003) and Roberts (2006).…”

Section: Introductionmentioning

confidence: 99%

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Cutoff periods of magnetoacoustic waves in the solar atmosphere

Kraśkiewicz¹,

Murawski²,

Musielak

2019

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We perform numerical simulations of magnetoacoustic waves (MAWs) in the solar atmosphere, which is gravitationally stratified and structured by either vertical or horizontal uniform magnetic fields. These waves are excited by a monochromatic driver that operates in the photosphere. We show that the gradients of the atmospheric parameters lead to filtering of the waves through the solar atmosphere and to variations of the dominant wave period with height. We use these variations to determine a local cutoff period, which shows a good agreement with the previously obtained analytical and numerical results in an isothermal solar atmosphere. In our numerical simulations, the propagation of MAWs in a more realistic model of the solar atmosphere is considered, and the obtained results demonstrate that the waves with periods higher than a local cutoff wave period are strongly reflected and become evanescent with height, while the waves with shorter wave periods are propagating, and may even reach the solar corona. Some of the evanescent waves may also tunnel and reach the atmospheric heights that would not be otherwise accessible to them. An important result of our study is excitation of chromospheric oscillations with periods equal to the period that is comparable to the observed solar chromospheric oscillations. Implications of our theoretical predictions are discussed.

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