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1.
To make a long-term prediction of the solar cycle in a standard way (GOST 25645.302-83), it is necessary to know the instant of the activity minimum onset, the determination of which is difficult during the decline stage of the previous cycle. The dependence of the long-term prediction error on the time of shift (t) relative to the solar activity minimum instant (i.e., the situation when a certain time before the minimum onset, rather than the time of this minimum, is the initial point of calculations) has been studied. It has been indicated that one should not know the exact time of the activity minimum onset in order to make prediction according to GOST, and such a prediction can be performed with an approximately identical error if the lead time is t ～ 1 year and more relative to the activity minimum onset. An analysis of the dependence of prognostic W max values on t for cycles 18–23 indicated that prognostic W max values are overestimated at small (to ～ 1 year) uncertainties in the time of activity minimum onset. It has been obtained that W max = 96 ± 13 for cycle 24 on the assumption that this cycle began in April 2007. 相似文献
2.
Geomagnetism and Aeronomy - We develop an approach to create a model of the solar extreme ultraviolet spectrum in the wavelength range responsible for dissociation of molecular oxygen... 相似文献
3.
The paper presents data on flux variations of ionizing EUV radiation for wavelengths shorter than 130 nm and in L-alpha hydrogen line on the basis of measurements performed on-board a Russian Earth-orbiting and interplanetary spacecrafts in the period since 1978 to 1997. These data were received by using common heritage instrumentation installed on four PROGNOZ satellites, INTERBALL-1, PHOBOS, and the geosynchronous meteorological satellite ELECTRO. Though the time series of observations is not continuous, it gives a possibility to estimate flux variations in certain periods of time and during 11–year cycle. During quiet periods of solar activity (except for flares) a level of diurnal variations is rather low, it being equal to about 3%. Radiation changes in L-alpha line from maximum to minimum in an 11–year cycle of solar activity achieves 200% and increases in the range of short waves. Data measured onboard the Russian satellites are compared with data obtained by Solar Mesospheric Explorer. 相似文献
4.
The results of measuring UV radiation onboard the CORONAS-F spacecraft during solar flares in 2001–2003 are considered. Some conclusions from the analysis of variations of solar-flare emission in several spectral intervals, namely, in soft X-rays, in the 10-to 130-nm range, and in the band near 120 nm, are discussed. The data were obtained by the VUSS-L and SUFR instruments. Time and energy characteristics of flares recorded onboard the CORONAS-F spacecraft are compared to the GOES measurements in the interval 0.1–0.8 nm and to the SOHO measurements of UV radiation in the 26-to 34-nm band. In particular, it is demonstrated that UV radiation is generated several (1–10) minutes before X-ray emission for most flares considered in the study. It is shown that the energy of flare emission in the extreme ultraviolet is usually not greater than ～10% of its preflare level and that energy fluxes in different wavelength ranges are related by a power law. Such an analysis makes it possible to better understand the mechanism of flare development. 相似文献
5.
A. A. Nusinov T. V. Kazachevskaya V. V. Katyushina K. V. Kuimov O. I. Bugaenko V. A. Slemzin N. I. Lebedev 《Solar System Research》2006,40(4):348-353
The CORONAS-F spacecraft crossed the zone of the ring solar eclipse three times on May 31, 2003. A considerable decrease in solar radiation was detected by the spacecraft instruments for these moments. The passages through the eclipse zone were registered by the VUSS instrument, which measured the shortwave solar radiation flux near the hydrogen Lyman alpha line, and by the DIFOS instrument, which was sensitive to infrared, visible, and near-ultraviolet radiation. The eclipse is also clearly seen in solar images obtained by the X-ray SPIRIT telescope. Some details of measurement results are discussed. 相似文献
6.
A. A. Nusinov 《Geomagnetism and Aeronomy》2008,48(4):472-478
It has been proposed to use the cumulative indices, applicable when macroeconomic processes are analyzed, to study long-term trends in different heliogeophysical factor, which vary under the action of cyclic changes in solar activity. It has been indicated that trends of the UV intensity in the Lyman-α line (reconstructed based on the ionospheric data) are almost absent for the period 1957–2004. 相似文献
7.
A. A. Nusinov T. V. Kazachevskaya S. N. Kuznetsov I. N. Myagkova B. Yu. Yushkov 《Solar System Research》2006,40(4):282-285
The results of simultaneous measurements of variations of UV radiation (in a band near the hydrogen Lα line, 121.6 nm) and hard X-ray and gamma-ray radiation (50 keV-200 MeV) performed by the VUSS-L and SONG instruments, respectively, onboard the CORONAS-F spacecraft are presented for periods of solar flares. Variations in the Lα ultraviolet radiation during the impulsive phase of a flare are shown to be synchronous with those of hard X-ray radiation. Temporal variations of UV and X-ray fluxes correspond to the progressive heating of higher and higher regions of the solar atmosphere and the energy transfer from the lower layers of the solar atmosphere to the coronal areas of flare regions. The energy of electrons in beams arising during the impulsive phase of flares can be as high as 500 keV. The velocity of the energy propagation from the regions of its release to the upper layers of the solar atmosphere can reach several tens of kilometers per second. 相似文献
8.
T. V. Kazachevskaya A. A. Nusinov V. V. Katyushina D. A. Gonjyukh 《Solar System Research》2008,42(4):359-362
The CORONAS-I and CORONAS-F data on variations in the ionizing shortwave ultraviolet (UV) solar radiation (EUV radiation) at wavelengths of less than 130 nm and near the H Lyman-alpha line are presented. The CORONAS-I data refer to the period close to solar minimum (the index F 10.7 = 80?100), and the CORONAS-F measurements were held close to solar maximum (F10.7 = 140?280). The UV data are compared to those from the UARS and SOHO satellites and to the results obtained from the ionospheric measurements of ionosphere critical frequencies. 相似文献
9.
A. A. Nusinov T. V. Kazachevskaya V. V. Katyushina P. M. Svidskii Yu. N. Tsigel'nitskii D. A. Gonyukh A. N. Afanas'ev S. I. Boldyrev D. V. Lisin A. I. Stepanov 《Solar System Research》2005,39(6):470-478
The paper presents a brief review of the instruments developed for measurement of ionizing extreme UV solar radiation at wavelengths of less than 130 nm onboard the CORONAS-I and CORONAS-F satellites and summarizes the observation data. The main goal of the study was to obtain information concerning variations of fluxes of solar radiation and solar flares at various wavelengths in the extreme ultraviolet. SUFR radiometers based on the thermoluminescent method were mounted onboard both CORONAS satellites (CORONAS-I and CORONAS-F). They performed measurements at λ < 130 nm. Spectral measurements in the 30.4-nm line were made by the photoelectronic spectrometer VUSS tested on CORONAS-I. Spectral measurements in the waveband including the H Lα line (121.6 nm) were conducted by the VUSS-L instrument (a Lyman alpha spectrophotometer) onboard the CORONAS-F satellite. The basic characteristics of the instruments, which were supposed to be used in a system of space weather monitoring on patrol satellites of the hydrometeorological service of Russia, are presented. The main data on the solar radiation flux at λ < 130 nm for minimum and maximum solar activity are given for quiet conditions and during solar flares. 相似文献
10.
T. V. Kazachevskaya S. I. Avdushin D. A. Gonukh A. I. Lomovsky A. A. Nusinov P. M. Svidsky Yu. N. Tsigelnitsky V. N. Oraevsky I. M. Kopaev S. I. Boldirev 《Solar physics》1998,177(1-2):175-180
There are presented data on solar emission variations in the extreme ultraviolet range?inebreak (λ < 130 nm) which were obtained on board the CORONAS-I satellite during the solar activity minimum epoch in 1994. Based on the thermoluminescent technique, the measurements were performed using the SUFR (Solar Ultraviolet Radiometer) equipment for recording the solar emission flux at λ < 130 nm. The technique provides absolute measurements. The intensity of the Heii 30.4 nm line emission was also measured on board the CORONAS by means of the Vacuum Ultraviolet Solar Spectrometer (VUSS), which uses gas-photoelectron energy and intensity analysis to register the spectrum. The characteristics of both devices are given, as well as calibration methods and the main results. The observation period may be characterized by a very low activity level. The solar flux in the region λ < 130 nm was 7.5–8 erg cm-2 s-1, the Lα line intensity was～ (3.3 –3.7) × 1011 photon cm-2 s-1 and the Heii (30.4 nm) line intensity was (6–7.5) × 109 photon cm-2 s-1. Intensive solar flares were not registered during the period of observation. During the flare of B4.5 X-ray class (30 June 1994, 01:08 UT), an increase of flux of ～ 15% was registered in the range λ < 130 nm. 相似文献