TY - JOUR

T1 - Dynamics and characteristics of waves in the zebra radio source

AU - Yasnov, L.V.

AU - Karlický, Marian

N1 - Publisher Copyright: © 2022, The Author(s), under exclusive licence to Springer Nature B.V.

PY - 2022/3

Y1 - 2022/3

N2 - We analyzed the 17 August 1998 zebra event and showed that some quasi-periodic oscillations modulate the zebra-stripe frequencies. We determined the period of these oscillations as P n= 2.01 ± 0.03 (in numbers of zebra stripes) and as P f= 11.8 ± 0.17 MHz. In the first part of the analyzed zebra, we found a stable density wave that slowly propagated with the frequency drift less than 0.4 MHz s −1. Then, a stationary density wave appeared followed by a transformation of the waves to ones with longer periods. These long-period waves were recorded before and after the time interval when no zebra stripes were observed. We interpreted these density waves as magnetosonic waves. We calculated their wavelength and propagating velocity, considering two types of density models of the solar atmosphere. We also estimated the characteristic density and magnetic-field strength as N≈ 9.2 × 10 8 cm −1 and B≈0.73G, respectively. We found similar velocities derived from drifts of the density wave and velocities calculated from the density and magnetic-field strength considering gyro-harmonic numbers of zebra stripes.

AB - We analyzed the 17 August 1998 zebra event and showed that some quasi-periodic oscillations modulate the zebra-stripe frequencies. We determined the period of these oscillations as P n= 2.01 ± 0.03 (in numbers of zebra stripes) and as P f= 11.8 ± 0.17 MHz. In the first part of the analyzed zebra, we found a stable density wave that slowly propagated with the frequency drift less than 0.4 MHz s −1. Then, a stationary density wave appeared followed by a transformation of the waves to ones with longer periods. These long-period waves were recorded before and after the time interval when no zebra stripes were observed. We interpreted these density waves as magnetosonic waves. We calculated their wavelength and propagating velocity, considering two types of density models of the solar atmosphere. We also estimated the characteristic density and magnetic-field strength as N≈ 9.2 × 10 8 cm −1 and B≈0.73G, respectively. We found similar velocities derived from drifts of the density wave and velocities calculated from the density and magnetic-field strength considering gyro-harmonic numbers of zebra stripes.

KW - Fine structure

KW - Radio bursts

KW - Sun: flares

KW - Zebra pattern

KW - INSTABILITY

KW - FINE-STRUCTURE

KW - SOLAR

KW - PATTERNS

KW - EMISSION

KW - REGION

UR - http://www.scopus.com/inward/record.url?scp=85126527579&partnerID=8YFLogxK

UR - https://www.mendeley.com/catalogue/40b5cdc9-43cf-3f4d-b829-931f9707227b/

U2 - 10.1007/s11207-022-01950-5

DO - 10.1007/s11207-022-01950-5

M3 - Article

VL - 297

JO - Solar Physics

JF - Solar Physics

SN - 0038-0938

IS - 3

M1 - 35

ER -