Comprehensive studies of solar activity on the CORONAS-F satellite

Oraevsky, V. N.; Sobelman, Igor I.

doi:10.1134/1.1484141

Cited by 35 publications

(17 citation statements)

References 1 publication

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Computation of the FPS pattern has been followed successfully allowing to correct for this effect. This work was done by Phillips (1994) and recently by Sylwester et al (2004a), for the Yohkoh BCS and RESIK instrumentation setups, respectively. It should be noted that the mechanism of the effect is not a scaling law (like a sensitivity change) but a redistribution of counts from one location, inaccessible due to the finite table, to another.…”

Section: Detectorsmentioning

confidence: 99%

See 1 more Smart Citation

Resik: A Bent Crystal X-ray Spectrometer for Studies of Solar Coronal Plasma Composition

et al. 2005

Self Cite

View full text Add to dashboard Cite

We describe the RESIK (REntgenovsky Spektrometr s Izognutymi Kristalami) instrument, consisting of two double-channel X-ray spectrometers, designed to observe solar active region and flare plasmas. RESIK is one of the instruments making up the scientific payload of the Russian CORONAS-F solar mission. The uncollimated spectrometer uses two silicon and two quartz bent crystals observing flare, active region and coronal spectra in four wavelength bands with a resolving power (λ/ λ) of ∼1000. The wavelength coverage, 3.3 -6.1Å, includes emission lines of Si, S, Cl, Ar, and K and in the third diffraction order, the wavelength range includes He-like Fe lines (1.85Å) and Ni lines (1.55Å) with dielectronic satellites, emitted during intense, hot flares. The instrument is believed to be the best calibrated space-borne crystal spectrometer flown to date. The spectrometer dynamically adjusts the data gathering intervals from 1 s to 5 minutes, depending on the level of solar X-ray emission at the time of observation. The principal aims of RESIK are the measurements of relative and absolute element abundances in the emitting plasma and the temperature distribution of plasma (differential emission measure) over the temperature interval 3 and 50 MK. This paper summarizes the scientific objectives of RESIK and describes the design, characteristics, and performance of the instrument.

show abstract

Section: Detectorsmentioning

confidence: 99%

“…The payload carries also instruments sensing the immediate particle environment. Further details about the instruments and data acquisition are given by Oraevsky and Sobelman (2002) and may be found on the web site http://coronas.izmiran.rssi.ru/F/.…”

Section: The Coronas-f Spacecraftmentioning

confidence: 99%

Resik: A Bent Crystal X-ray Spectrometer for Studies of Solar Coronal Plasma Composition

et al. 2005

Self Cite

View full text Add to dashboard Cite

show abstract

“…The eruptive filament bifurcated and transformed into a large Y-shaped cloud, which moved from the region of bifurcation (Rb) to the South-West across the solar disk toward the limb. Figure 1 illustrates what has happened to the eruptive filament, as shown by the Hα images produced by the Kanzelhöhe Solar Observatory (KSO), the Extreme-ultraviolet Imaging Telescope (EIT; Delaboudinière et al, 1995), on board the Solar and Heliospheric Observatory (SOHO), and the Spectroheliographic X-ray Imaging Telescope (SPIRIT; Zhitnik et al (2002) and Slemzin et al (2005)), on board the Complex Orbital near-Earth Observations of Activity of the Sun (CORONAS-F) satellite (Oraevsky and Sobelman, 2002;Oraevsky et al, 2003).…”

Section: Introductionmentioning

confidence: 99%

A Challenging Solar Eruptive Event of 18 November 2003 and the Causes of the 20 November Geomagnetic Superstorm. III. Catastrophe of the Eruptive Filament at a Magnetic Null Point and Formation of an Opposite-Handedness CME

et al. 2014

View full text Add to dashboard Cite

Our analysis in Papers I and II (Grechnev et al., 2014, Solar Phys. 289, 289 and 1279) of the 18 November 2003 solar event responsible for the 20 November geomagnetic superstorm has revealed a complex chain of eruptions. In particular, the eruptive filament encountered a topological discontinuity located near the solar disk center at a height of about 100 Mm, bifurcated, and transformed into a large cloud, which did not leave the Sun. Concurrently, an additional CME presumably erupted close to the bifurcation region. The conjectures about the responsibility of this compact CME for the superstorm and its disconnection from the Sun are confirmed in Paper IV (Grechnev et al., Solar Phys., submitted), which concludes about its probable spheromak-like structure. The present paper confirms the presence of a magnetic null point near the bifurcation region and addresses the origin of the magnetic helicity of the interplanetary magnetic clouds and their connection to the Sun. We find that the orientation of a magnetic dipole constituted by dimmed regions with the opposite magnetic polarities away from the parent active region corresponded to the direction of the axial field in the magnetic cloud, while the pre-eruptive filament mismatched it. To combine all of the listed findings, we come to an intrinsically three-dimensional scheme, in which a spheromak-like eruption originates via the interaction of the initially unconnected magnetic fluxes of the eruptive filament and pre-existing ones in the corona. Through a chain of magnetic reconnections their positive mutual helicity was transformed into the self-helicity of the spheromak-like magnetic cloud.

show abstract

“…The SPIRIT telescopes onboard the CORONAS-F satellite (Oraevsky and Sobelman, 2002) have routinely observed the Sun in the EUV range 171-304 Å since August 2001. The most intense ion lines emitted from the transition region and the inner corona ( T ~ 0.03-2 MK) lie in this spectral region.…”

Section: Introductionmentioning

confidence: 99%

Observations of Solar EUV Radiation with the CORONAS-F/SPIRIT and SOHO/EIT Instruments

et al. 2005

View full text Add to dashboard Cite

The SPIRIT complex onboard the CORONAS-F satellite has routinely imaged the Sun in the 171, 175, 195, 284, and 304 Å spectral bands since August 2001. The complex incorporates two telescopes. The Ritchey-Chretien telescope operates in the 171, 195, 284, and 304 Å bands and has an objective similar to that of the SOHO /EIT instrument. The Herschel telescope obtains solar images synchronously in the 175 and 304 Å bands with two multilayer-coated parabolic mirrors. The SPIRIT program includes synoptic observations, studies of the dynamics of various structures on the solar disk and in the corona up to 5 solar radii, and coordinated observations with other spaceborne and ground-based telescopes. In particular, in the period 2002-2003, synoptic observations with the SPIRIT Ritchey-Chretien telescope were coordinated with regular 6-hour SOHO /EIT observations. Since June 2003, when EIT data were temporarily absent ( SOHO keyholes), the SPIRIT telescope has performed synoptic observations at a wavelength of 175 A. These data were used by the Solar Influence Data Analysis Center (SIDC) at the Royal Observatory of Belgium for an early space weather forecast. We analyze the photometric and spectral parameters of the SPIRIT and EIT instruments and compare the integrated (over the solar disk) EUV fluxes using solar images obtained with these instruments during the CORONAS-

show abstract

Comprehensive studies of solar activity on the CORONAS-F satellite

Cited by 35 publications

References 1 publication

Resik: A Bent Crystal X-ray Spectrometer for Studies of Solar Coronal Plasma Composition

Resik: A Bent Crystal X-ray Spectrometer for Studies of Solar Coronal Plasma Composition

A Challenging Solar Eruptive Event of 18 November 2003 and the Causes of the 20 November Geomagnetic Superstorm. III. Catastrophe of the Eruptive Filament at a Magnetic Null Point and Formation of an Opposite-Handedness CME

Observations of Solar EUV Radiation with the CORONAS-F/SPIRIT and SOHO/EIT Instruments

Contact Info

Product

Resources

About