Astronomical Observatory of Kharkov National University Department of Solar, Lunar and Planetary Physics
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1999-2004 Astronomical Institute of Kharkiv University. Department of Solar, Lunar and Planetary Physics

Kharkiv Multiwave Station of Solar Monitoring

Korokhin V., Akimov L., Beletsky S., Belkina I.,
Velikodsky Yu., Marchenko G., Shaparenko E.

Introduction

It is known that phenomena of solar activity have a greater influence on processes in magnetosphere and ionosphere of the Earth, on terrestrial weather conditions, health of people. It is necessary to take the activity into account for studying the problems of human ecology and environment. Modern station of solar monitoring provides with data the monitoring near-Earth space, radio communications, servicing the computer networks, electric networks, pipe-line transport. Data on solar activities are necessary for public health; they are used during cosmic projects.

Station of solar monitoring (SSM) on the base of the specroheliograph of Astronomical observatory of Kharkiv State University and CCD photo sensors allows to obtain digital images of the Sun regularly in any spectral band from 300 to 1200 nm with periodicity 0.5-2 minutes. In case of need after simple modernization it will be possible simultaneous obtaining images in several spectral ranges.

In the monitoring mode digital images of the Sun are processed in real-time regime, classified and put to the electronic databank. Consumers (scientists, interested organizations, astronomy amatours, observations requesters, etc.) can obtain the data from the databank via Internet.

Scientific tasks

SSM main purpose is solar activity monitoring. It is planned to carry out observing of the Sun simultaneously in the helium infrared line (1083 nm), the Balmer continuum of hydrogen (364 nm) and the H-alpha hydrogen line (656.3 nm) with periodicity 5-10 minutes (Belkina at al., 1996).

Images in the helium infrared line contain information about coronal holes (sources of solar winds) and other objects, which can be observed from space instruments only. Today only Kitt-Peak observatory (USA) regularly obtains such images.

H-alpha line observations are the most available way to fix solar flares and explosive processes in dark filaments and prominences. This allows to get data for the forecast of near-earth space condition.

Images obtaining in Balmer continuum is a new type of solar observing. It allows for the first time to obtain data about macroscopic heterogeneity of solar plasma density, about the statistics, dynamics and morphology of areas with increased electronic density (Kurochka at al., 1997).

Simultaneous observations in these spectral ranges with high time resolution allow to study the evolution of chromospheric flares and quick processes on different heights of solar atmosphere.

It allows to obtain in principal new data on physical characteristics of solar atmosphere and its activity, and to raise forecast quality for solar flares and other types of the solar activity.

Main features

- Easy tuneability. (It is possible to observe the Sun in any spectral range from 300 nm to 1200 nm in the monochromatic light. Band width is 0.0024 nm.)
- The Possibility of observations in several spectral bands simultaneously.
- High time resolution.
(Full image (1000x1000) of the Sun is obtained during 0.5-2 minutes.)
- The Spatial resolution is limited only by the atmosphere (approximately 2").
- Data processing and formalization are performed in real-time regime.
- Round-the-clock access to data through Internet.
- Carrying out the custom-tailored observations.

(Kharkiv Station of Solar Monitoting (KHASSM) in the Internet)

2002/06/08

 
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