共查询到20条相似文献，搜索用时 687 毫秒
1.
H.-J. Haubold S. Gottlber J. P. Mücket V. Müller B. Kmpfer 《Astronomische Nachrichten》1987,308(6):329-331
Implications from the available information on the supernova SN 1987 A are discussed for the supernova models. We derive an upper bound of 10–25 eV for the neutrino rest mass. 相似文献
2.
Basic characteristics of the “response” of underground neutrino detectors to the explosion of SN 1987A occurred on February 23, 1987, are presented. We discuss the evolution of our viewpoint on the interpretation of the results concerning the detection of neutrino radiation from the supernova over the past 20 years. 相似文献
3.
Gillian Pearce Bruce Patchett Jeremy Allington-Smith Ian Parry 《Astrophysics and Space Science》1988,150(2):267-271
We present the spectrum of the supernova SN1987L in NGC 2336 over the wavelength range 4000–9700 Å as recorded in one 500 s exposure on 20–21 October, 1987. This spectrum was taken using the new Faint Object Spectrograph on the 4.2 m William Herschel Telescope (WHT) at the Observatorio del Roque de los Muchachos.We conclude that SN1987L was a type Ia supernova, and approximately 100 days post maximum at the time of the observation. 相似文献
4.
An approximate value for the energy radiated by supernova 1987A is derived by integrating the curve which represents the intensity of the object as a function of time. The optical faintness of the supernova becomes evident when comparing this amount with other possible sources of energy. 相似文献
5.
D. N. Voskresensky A. V. Senatorov B. Kaempfer H. J. Haubold 《Astrophysics and Space Science》1987,138(2):421-424
It is argued that the neutrino bursts registered on February 23.316 UT, 1987 signalized the transition of a fresh-borne neutron star into a superdense state. The neutron star is supposed to be formed approximately five hours before at February 23.12 UT in the supernova SN 1987a in the Large Magellanic Cloud. 相似文献
6.
Luis A. Milone S. Paolantonio V. Briggi D. Mendicini E. Minniti 《Astrophysics and Space Science》1988,150(2):291-297
V andB light curves for supernova 1987A covering some 120 days from the outburst are here presented and discussed; they are shown to be rather atypical for a type II supernova. The absolute magnitude at maximum brightness is also analyzed, and after applying a correction for interstellar absorption we obtainM
V, max, 0
=–16.1, andM
B, max, 0
=–14.7; is is then concluded that 1987A is a supernova quite fainter than average. A comparison with other known supernova is made and some similarity is found with peculiar objects such as 1948B in NGC 6946, and probably, 1909 A in M 101.Research supported in part by SECyT and CONICOR. 相似文献
7.
We investigate the evaporation and condensation of corundum and silicon carbide grains around the supernova SN1987A. We predict the time after outburst of the interaction of the condensed dust with pre-existing dust, with a view to undertaking observations with future instrumentation such as the Infra-Red Space Observatory. 相似文献
8.
The influence of the results of the grand unified theory of interactions on the formation of black holes is discussed and compared with the observations of the supernova 1987a. 相似文献
9.
Zhao Gang Zhao Yong-heng Huang Jia-sheng Feng Long-long Huang Ke-liang Peng Qiu-he Lu Tan 《Chinese Astronomy and Astrophysics》1988,12(4):294-297
We carried out a Monte Carlo simulation calculation on the observed data of neutrino events of the supernova SN1987A. Our results show that the best value for the rest-mass of neutrino is 3–4 eV. We also calculated the light curve of the neutrino bursts and the energy spectrum.Our results impose constraints on the rest-mass of neutrino and the mass of the precursor of SN 1987A. 相似文献
10.
Most current supernova theories state that this phenomenon lasts a few seconds and ends with a bigfinal explosion.However, these theories do not take into account several experimental results obtained with neutrino and gravitational wave detectors during the explosion of SN1987A, the only supernova observed in a nearby galaxy in modern age. According to these experimental results the phenomenon is much more complex that envisaged by current theories, and has a duration of several hours. Indeed, SN1987A exploded on February 23, 1987, and two neutrino bursts, separated by 4.7 hours were detected: the first one at 2h 52m UT and the second one at 7h 35m UT. Furthermore, correlations between the neutrino and two gravitational wave detectors, ignored by most of the scientific community, were observed during the longer collapse time. Since the current standard theories, based on some rough simplifications, are a clear example of an Aristotelian attitude, still present in our days, we believe that a more Galilean attitude is necessary, being the only correct way for the progress of science. 相似文献
11.
In this paper the contributions of various radioactive substances (56Co, 57Co, 44Ti and 22Na) in the envelope of the supernova SN 1987A to the evolution of the bolometric luminosity are calculated and the several types of radiation, which may probably exist in the interior neutron star, as well as their contributions to the bolometric luminosity are investigated. After comparison of the results of calculation with the observation of CTIO and ESO, it is believed that after about 900 days the nuclear decay energy is no longer the unique energy source which determines the bolometric luminosity evolution of SN 1987A, that the radiation coming from the interior neutron star begins to play a dominating role in the bolometric luminosity evolution and that the most important mechanism of radiation of the neutron star is accretion. 相似文献
12.
L. A. L. Da Silva 《Astrophysics and Space Science》1990,165(2):255-260
A comparison is made of the light and colour curves of the SN 1987A in the first 280 days with the mean properties of type II supernovae. The conclusion is that even though it has H lines, and was not a typical type II supernova, but a peculiar object from a photometric point of view. The implications for inclusion of SN 1987A in the context of the usual Minkowski-Zwicky classification are explicitly discussed. 相似文献
13.
Providing an early warning of galactic supernova explosions from neutrino signals is important in studying supernova dynamics and neutrino physics. A dedicated supernova trigger system has been designed and installed in the data acquisition system at Daya Bay and integrated into the worldwide Supernova Early Warning System (SNEWS). Daya Bay’s unique feature of eight identically-designed detectors deployed in three separate experimental halls makes the trigger system naturally robust against cosmogenic backgrounds, enabling a prompt analysis of online triggers and a tight control of the false-alert rate. The trigger system is estimated to be fully sensitive to 1987A-type supernova bursts throughout most of the Milky Way. The significant gain in sensitivity of the eight-detector configuration over a mass-equivalent single detector is also estimated. The experience of this online trigger system is applicable to future projects with spatially distributed detectors. 相似文献
14.
15.
David A. Noever 《Astrophysics and Space Science》1994,220(1):65-74
Near supernova 1987a, the rare honeycomb structure of 20–30 galactic bubbles measures 30 × 90 light years. Its remarkable regularity in bubble size suggests a single-event orgin which may correlate with the nearby supernova. To test the honeycomb's regularity in shape and size, the formalism of statistical crystallography is developed here for bubble sidedness. The standard size-shape relations (Lewis's law, Desch's law, and Aboav-Weaire's law) govern area, perimeter and nearest neighbor shapes. Taken together, they predict a highly non-equilibrium structure for the galactic honeycomb which evolves as a bimodal shape distribution without dominant bubble perimeter energy. 相似文献
16.
The neutrino burst from Supernova 1987A detected by Mont Blanc, Kamiokande II, IMB, and BAKSAN have been studied by Jurkevich's mathematical technique of search for periodicities. It is found that all the data exhibit 11±0.2 ms period. There are also other periods, but they are almost exact multiples of 11 ms. We suggests that the 11 ms period is the pulsation period of the neutron core of the supernova remnant. From the observed period of neutrino data it is also possible to predict the masses of the neutrinos. 相似文献
17.
A. Pastorello E. Baron D. Branch L. Zampieri M. Turatto M. Ramina S. Benetti E. Cappellaro M. Salvo F. Patat A. Piemonte J. Sollerman B. Leibundgut G. Altavilla 《Monthly notices of the Royal Astronomical Society》2005,360(3):950-962
We present spectroscopic and photometric observations of the peculiar Type II supernova (SN) 1998A. The light curves and spectra closely resemble those of SN 1987A, suggesting that the SN 1998A progenitor exploded when it was a compact blue supergiant. However, the comparison with SN 1987A also highlights some important differences: SN 1998A is more luminous and the spectra show bluer continua and larger expansion velocities at all epochs. These observational properties indicate that the explosion of SN 1998A is more energetic than SN 1987A and more typical of Type II supernovae. Comparing the observational data with simulations, we deduce that the progenitor of SN 1998A was a massive star (∼25 M⊙ ) with a small pre-supernova radius (≲6 × 1012 cm) . The Ba ii lines, unusually strong in SN 1987A and some faint II-P events, are almost normal in the case of SN 1998A, indicating that the temperature plays a key role in determining their strength. 相似文献
18.
《Physics and Chemistry of the Earth, Part C: Solar, Terrestrial & Planetary Science》1999,24(5):579-581
In the ejecta of a supernova, the temperature of the created grains differs from that of the gas due to the radiation from the star. We investigated the grain formation in the supernova using a developed new nucleation rate where the temperature difference between the gas and the grains is taken into account. If the temperature of the grains is higher than that of the gas, the nucleation process does not occur when the gaseous temperature attains the condensation temperature. As a result we found that the temperature difference between the gas and the grains in SN1987A is about 50–200K which leads that the nucleation is delayed for about 20–100 days. 相似文献
19.
We present the results of our observations of two types of Galactic supernova remnants with the ShALON mirror Cherenkov telescope:
the plerion Crab Nebula and the shell-type supernova remnants Cassiopeia A and Tycho. The experimental data have confirmed
the prediction of the theory about the hadronic generation mechanism of very high energy (0.8–100 TeV) gamma rays in Tycho’s
supernova remnant. The data obtained suggest that the very high energy gamma-ray emission in the objects being discussed is
different in origin. 相似文献
20.
We present a real-time supernova neutrino burst monitor at Super-Kamiokande (SK). Detecting supernova explosions by neutrinos in real time is crucial for giving a clear picture of the explosion mechanism. Since the neutrinos are expected to come earlier than light, a fast broadcasting of the detection may give astronomers a chance to make electromagnetic radiation observations of the explosions right at the onset. The role of the monitor includes a fast announcement of the neutrino burst detection to the world and a determination of the supernova direction. We present the online neutrino burst detection system and studies of the direction determination accuracy based on simulations at SK. 相似文献