Onset Time of the GLE 72 Observed at Neutron Monitors and its Relation to Electromagnetic Emissions

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F61389005%3A_____%2F19%3A00503152" target="_blank" >RIV/61389005:_____/19:00503152 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.1007/s11207-019-1407-9" target="_blank" >https://doi.org/10.1007/s11207-019-1407-9</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1007/s11207-019-1407-9" target="_blank" >10.1007/s11207-019-1407-9</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Onset Time of the GLE 72 Observed at Neutron Monitors and its Relation to Electromagnetic Emissions

Popis výsledku v původním jazyce

The maximum increase at high-latitude near-sea-level NMs was approximate to 6-7% (2-min averages), greater with better time resolution. A scatter plot of the maximum increase of the GLE versus solar energetic-particle (SEP, proton) flux > 100 MeV shows one of the softest spectra among GLEs relative to the SEP fluxes. However, at two high-mountain middle-latitude NMs the increase was approximate to 1%, indicating the possibility of proton acceleration up to 6 GeV. Among the analyzed NM data the FSMT NM shows the earliest and the rather high increase between 16:06-16:08 UT. This indicates an anisotropy in the first phase of the GLE event. We calculate the acceptance cones of several NM stations at high latitudes and contours of pitch angles corresponding to the interplanetary magnetic field (IMF). When employing the available data we find that pion-decay.-ray emission onset is in accordance with the time of the main flare energy release. The observed time interval of the impulsive burst of >100 MeV gamma-ray emission probably corresponds to the time of a turbulent current sheet creation. The observed location of the impulsive burst pion-decay emission source coincides with the active region and the cusp-shaped structure. It seems that models assuming sub-relativistic proton production beginning in a turbulent reconnecting current sheet are consistent with the observations. If these particles were released from the Sun during a type III emission with a pion-decay maximum at 16:00:30 +/- 30 UT, we get a plausible path length equal to 1.5 +/- 0.3 AU of the particles responsible for the onset of the SEP event and GLE. The time lag of GLE 72 corresponds to the most probable interval of the time difference between GLE onset and main flare energy release. Although other scenarios are not excluded we attribute the protons that create the pion-decay emission and the protons responsible for the GLE and SEP event onset to a general population of accelerated particles.

Název v anglickém jazyce

Onset Time of the GLE 72 Observed at Neutron Monitors and its Relation to Electromagnetic Emissions

Popis výsledku anglicky

The maximum increase at high-latitude near-sea-level NMs was approximate to 6-7% (2-min averages), greater with better time resolution. A scatter plot of the maximum increase of the GLE versus solar energetic-particle (SEP, proton) flux > 100 MeV shows one of the softest spectra among GLEs relative to the SEP fluxes. However, at two high-mountain middle-latitude NMs the increase was approximate to 1%, indicating the possibility of proton acceleration up to 6 GeV. Among the analyzed NM data the FSMT NM shows the earliest and the rather high increase between 16:06-16:08 UT. This indicates an anisotropy in the first phase of the GLE event. We calculate the acceptance cones of several NM stations at high latitudes and contours of pitch angles corresponding to the interplanetary magnetic field (IMF). When employing the available data we find that pion-decay.-ray emission onset is in accordance with the time of the main flare energy release. The observed time interval of the impulsive burst of >100 MeV gamma-ray emission probably corresponds to the time of a turbulent current sheet creation. The observed location of the impulsive burst pion-decay emission source coincides with the active region and the cusp-shaped structure. It seems that models assuming sub-relativistic proton production beginning in a turbulent reconnecting current sheet are consistent with the observations. If these particles were released from the Sun during a type III emission with a pion-decay maximum at 16:00:30 +/- 30 UT, we get a plausible path length equal to 1.5 +/- 0.3 AU of the particles responsible for the onset of the SEP event and GLE. The time lag of GLE 72 corresponds to the most probable interval of the time difference between GLE onset and main flare energy release. Although other scenarios are not excluded we attribute the protons that create the pion-decay emission and the protons responsible for the GLE and SEP event onset to a general population of accelerated particles.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10509 - Meteorology and atmospheric sciences

Projekt

<a href="/cs/project/EF15_003%2F0000481" target="_blank" >EF15_003/0000481: Centrum výzkumu kosmického záření a radiačních jevů v atmosféře</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2019

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Solar Physics

ISSN

0038-0938

e-ISSN

—

Svazek periodika

294

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

NL - Nizozemsko

Počet stran výsledku

18

Strana od-do

22

Kód UT WoS článku

000458689400002

EID výsledku v databázi Scopus

2-s2.0-85061477592