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1.
The behaviour of the flare in the period of enhancement and maximum of hard X-ray, microwave and decimetric type IV continuum is analysed. The elongation of the H ribbons and microwave source disclose that the energy release site was shifting through a system of loops with a velocity less than 200 km s-1, and that the energy was carried down the field lines with a velocity of about 1000 km s-1, implying the thermal conduction front mechanism of energy transport. Several processes of energy release are considered and it is concluded that an explanation in terms of succeeding interactions of neighbouring loops, involving fast reconnection of their poloidal components is in best agreement with the observations.Proceedings of the Second CESRA Workshop on Particle Acceleration and Trapping in Solar Flares, held at Aubigny-sur-Nère (France), 23–26 June, 1986. 相似文献
2.
Warmuth Alexander Hanslmeier Arnold Messerotti Mauro Cacciani Alessandro Moretti Pier Francesco Otruba Wolfgang 《Solar physics》2000,194(1):103-120
NOAA 8210 has been a region showing a remarkable level of activity well before solar maximum. Dominated by a large, rapidly rotating spot, it produced several intense flares during its disk passage at the end of April–beginning of May 1998. We examine the development of AR 8210 in H and white light (WL) and study the evolution of its complex magnetic topology. While the other principal flares are briefly reviewed, the great X1.1/3B flare of 2 May, which was observed at Kanzelhöhe Solar Observatory during a SOHO/UVCS ground support campaign, is studied in detail. This event has been documented in full-disk H and Na-D intensitygrams, Dopplergrams, and magnetograms, with a time cadence of one minute each. The flare was associated with a CME and produced significant geomagnetic effects. Furthermore, we point out the perspectives for our planned Flare Monitoring and Alerting System, since the two new instruments (Magneto-Optical Filter and Digital H camera), which made their first operational run with the campaign, are crucial components for this program. 相似文献
3.
M. Messerotti 《Earth, Moon, and Planets》2009,104(1-4):51-54
Observations and theoretical analyses indicate that solar radio noise can affect radio communications and GPS operations. In this work, we present a statistics relevant to the period 2000–2003 derived from the data recorded by the Trieste Solar Radio System (TSRS) and we stress the importance of precise radio flux measurements as pointed out by a comparison of tenflare catalog data with the TSRS ones for the period 2005–2006. 相似文献
4.
During the early stages of the study of the origin of life, not enough attention was paid to the question of the correlation
of chemical evolution on Earth and the all-important evolution of the still-to-be understood early Sun. Today, due to the
advent of a significant fleet of space missions and the possibility of performing experiments in the International Space Station
(ISS), a meaningful study begins to be possible concerning factors that led to an early onset of life on Earth. We wish to
review and update recent work concerning the frontier between Space Weather (SpW) and Astrobiology. We argue that the present
robust programs of various space agencies reinforce our hope for a better understanding of the bases of Astrobiology. Eventually,
with a more realistic model of the Sun, more reliable discussions of all the factors influencing the origin of life on Earth,
and hence Astrobiology, will be possible. 相似文献
5.
The time profile of two sets of isolated type III bursts, observed in the meter wavelength range at the Trieste Astronomical Observatory, was analyzed using a Fourier transform technique in order to accurately determine the decay constant of the exponential phase and to derive the exciter time profile. The decay constant () was found to be correlated with the exciter duration (D
e
), suggesting that the damping of plasma waves is not of collisional origin and confirming results obtained by previous authors at lower frequencies. In particular, two distributions can be identified in the ( – D
e
) plane and fitted by two nearly parallel lines, which could be the signature of different decay processes. Moreover, the damping constant observed at higher frequencies (327 and 408 MHz) has the same dependence on exciter duration as that at the lower frequency (237 MHz), also in disagreement with the collisional hypothesis. 相似文献
6.
A prime objective of this experiment was to determine whether type I or IV sources at 333 MHz contain features of small (arc sec) scale. With the VLA, our resolution was better than 4. However, we never observed any structure of size smaller than about 30, with the typical source sizes being between about 40 and 90.Many observations were simultaneous with the Trieste Astronomical Observatory records at 327 MHz. The observations were made on two days in November 1988. On 8 November the observations were of a type I storm about two hours after a major flare. On 14 November they were mostly of the main phase of a type IV event, including pulsations of a kind rarely seen, strongly circularly polarized, and having a well-defined period of about 12 s. The size of the pulsating source was about 40 by 60, and the brightness temperature was about 109 K. We compare these pulsations with those observed earlier. 相似文献
7.
V. Ruždjak M. Messerotti M. Nonino A. Schroll B. Vršnak P. Zlobec 《Solar physics》1987,111(1):103-111
We studied 24 spotless flares of Ha importance 1 which occurred during the 21st cycle of solar activity. The spotless flares could be grouped in three categories according to their location and time history of the associated active region. Our association of the flares with radio events was based on relative timing and on the flare importances. Weak microwave gradual rise and fall events were frequently recorded during the occurrence of the spotless flares. A few flares from our sample could be associated with impulsive and complex microwave bursts. Only in one case an association of a spotless flare with a significant metric type II/IV event seems to be justified.Proceedings of the Second CESRA Workshop on Particle Acceleration and Trapping in Solar Flares, held at Aubigny-sur-Nère (France), 23–26 June, 1986. 相似文献
8.
Out of 120 solar type IV events recorded at the Trieste Astronomical Observatory, we have selected 15 groups of spike bursts. We analyze their properties, concentrating on the characteristics of their polarization. We find that the polarization of the spikes varies over a wide range, but that within a particular group of spikes it remains almost constant. Sometimes groups of spikes with different degrees of polarization occur almost contemporaneously, probably indicating that more than one source is active at nearly the same time.Occasionally spike bursts accompany type III bursts. Then, unlike the case with type IV-associated events, the polarization of the spikes varies greatly.Proceedings of the Workshop on Radio Continua during Solar Flares, held at Duino (Trieste), Italy, 27–31 May, 1985. 相似文献
9.
We studied the properties of fine structures in 23 type II bursts recorded at the Trieste Astronomical Observatory at frequencies above 200 MHz.The lifetime of a single fine structure is a fraction of a second. The ratio of fine structures intensity vs bulk flux density is different in different type II bursts and it changes during the evolution of a single event; the reported maximum ratio is 3. The polarization of fine structures is nearly the same during the lifetime of an event. There is also no essential difference in polarization between fine structures and bulk emission; this holds also for an example of high-polarization (about 80%) event.At frequencies lower than 200 MHz the analogy between herringbone structure and type III bursts is frequently mentioned in the literature. From the observations we studied, it results, however, that the time profile of single fine-structure elements and their polarization are substantially different from the morphology of type III bursts.The observed fine structures and their characteristics are discussed in the framework of the model by Holman and Pesses (1983).Paper presented at the 4th CESRA Workshop in Ouranopolis (Greece) 1991. 相似文献
10.
The organization and activities of the international initiative named Electronic Geophysical Year (eGY), promoted by the International Union for Geodesy and Geophysics (IUGG) are outlined as synergetic to the other initiatives as the International Heliophysical Year (IHY). 相似文献