Investigation of Hot X-Ray Points (HXPs) Using Spectroheliograph Mg xii Experiment Data from CORONAS-F/SPIRIT

Details Investigation of Hot X-Ray Points (HXPs) Using Spectroheliograph Mg xii Experiment Data from CORONAS-F/SPIRIT Investigation of Hot X-Ray Points (HXPs) Using Spectroheliograph Mg xii Experiment Data from CORONAS-F/SPIRIT

Feb 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012soph..276...97r&link_type=abstract

Solar Physics, Volume 276, Issue 1-2, pp. 97-112

Physics

Corona, Active, Flares, Microflares And Nanoflares, Spectral Line, Broadening

Scientific paper

Observations in the Mg xii 8.42 Å line onboard the CORONAS-F satellite have revealed compact high temperature objects - hot X-ray points (HXPs) - and their major physical parameters were investigated. Time dependencies of temperature, emission measure, intensity, and electron density were measured for 169 HXPs. HXPs can be divided into two groups by their temperature variations: those with gradually decreasing temperature and those with rapidly decreasing temperature. HXP plasma temperatures lie in the range of 5 - 40 MK, the emission measure is 1045 - 1048 cm-3, and the electron density is above 1010 cm-3, which exceeds the electron density in the quiet Sun (108 - 109 cm-3). HXP lifetimes vary between 5 - 100 minutes, significantly longer than the conductive cooling time. This means that throughout a HXP’s lifetime, the energy release process continues, which helps to maintain its high temperature. A HXP’s thermal energy is not greater than 1028 erg, and the total energy which is released in HXPs does not exceed 1030 erg. HXPs differ in their physical properties from other flare-like microevents, such as microflares, X-ray bright points, and nanoflares.

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