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Large Magellanic Cloud

L. A. Marschall, The Supernova Story, Plenum Press, New York, 1989, 276 pp. P. Murdin, End in Fire The Supernova in the Large Magellanic Cloud, Cambridge University Press, 1990, 253 pp. [Pg.5]

The three broad classifications (elliptical, spiral and irregular) of star clusters that also cluster together to form the Local Group that contains the Milky Way and the Andromeda Galaxy, along with the Small and Large Magellanic Clouds... [Pg.38]

A neutrino burst was observed in the KAMIOKANDE-II detector on 23 February, 7 35 35 UT ( 1 minute) during a time interval of 13 seconds. The signal consisted of 11 electron events of energy 7.5 to 36 MeV, of which the first 2 point back to the Large Magellanic Cloud (LMC) with angles 18 18 and 15° 27 °. [Pg.335]

Scatter plot of the detected electron energy in MeV and the cosine of the angle between the measured electron direction and the direction of the Large Magellanic Cloud. The number to the left of each entry is the time sequential event number from Table I. The two projections of the scatter plot are also displayed. [Pg.342]

Analysis of Neutrino Burst from the Supernova in the Large Magellanic Cloud... [Pg.424]

The supernova 1987A in the Large Magellanic Cloud has provided a new opportunity to study the evolution of a young neutron star right after its birth. A proto-neutron star first cools down by emitting neutrinos that diffuse out of the interior within a minutes. After the neutron star becomes transparent to neutrinos, the neutron star core with > 1014 g cm-3 cools predominantly by Urea neutrino emission. However, the surface layers remain hot because it takes at least 100 years before the cooling waves from the central core reach the surface layers (Nomoto and Tsuruta 1981, 1986, 1987). [Pg.448]

Fig.6.83. Spectrum of the supernova 1987 A in the Large Magellanic Cloud, recorded 7 days after the explosion. The prominent lines are due to the hydrogen Balmer series, Doppler-shifted and broadened due to very high expansion velocities (lO.OOOkm/s). The line is partly seen also in emission. An insert shows narrow Na absorption lines due to cold gas clouds moving with different velocities along the line of sight [6.159]... Fig.6.83. Spectrum of the supernova 1987 A in the Large Magellanic Cloud, recorded 7 days after the explosion. The prominent lines are due to the hydrogen Balmer series, Doppler-shifted and broadened due to very high expansion velocities (lO.OOOkm/s). The line is partly seen also in emission. An insert shows narrow Na absorption lines due to cold gas clouds moving with different velocities along the line of sight [6.159]...
W. Hillebrandt, P. Hoflich The supernova 1987A in the Large Magellanic Cloud. Rep. Progr. Phys. 52, 1421 (1989)... [Pg.363]

See other pages where Large Magellanic Cloud is mentioned: [Pg.3]    [Pg.313]    [Pg.15]    [Pg.81]    [Pg.88]    [Pg.180]    [Pg.227]    [Pg.249]    [Pg.481]    [Pg.6]    [Pg.109]    [Pg.150]    [Pg.151]    [Pg.45]    [Pg.75]    [Pg.340]    [Pg.354]    [Pg.399]    [Pg.465]    [Pg.472]    [Pg.217]    [Pg.238]    [Pg.66]    [Pg.220]    [Pg.224]    [Pg.238]    [Pg.247]    [Pg.85]    [Pg.89]    [Pg.108]    [Pg.211]    [Pg.256]    [Pg.294]    [Pg.441]    [Pg.442]    [Pg.460]    [Pg.66]    [Pg.155]   
See also in sourсe #XX -- [ Pg.3 ]

See also in sourсe #XX -- [ Pg.6 , Pg.109 ]



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