Changes in the gravitational energy of galaxies during collisions

Sastry, K. S.

doi:10.1007/bf00642740

Cited by 14 publications

(2 citation statements)

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“…(i) the sense of polarization is LH for both components; (ii) P 2 > Pi (opposite to the relationship for RDPs); Proc./lS/»3(6)1979 (iii) the polarization values are somewhat higher than for RDPs. These results confirm the result of Sastry (1972) that the two components of drift pairs are polarized in the same sense. However, we have found a significant difference in degree of polarization between the two components of a pair which he did not report.…”

Section: Polarimeter Datasupporting

confidence: 90%

Position and Polarization of Solar Drift Pair Bursts

Suzuki

Gary

1979

Publ. Astron. Soc. Aust.

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Reverse drift pairs were first described by Roberts (1958) and later by Ellis (1969) and de la Nòe and Moller-Pedersen (1971). Figure 1 shows a 10-min section of the spectrograph record and the corresponding section of the polarimeter record. The figure contains several reverse drift pairs and illustrates the main features of RDPs, namely: (1) frequency drift rate of about 4 MHz s-1 (i.e. a factor of ~50 faster than Type lis and a factor of ~2 slower than type Ills); (2) drift to higher frequencies (i.e. opposite to that of Type II and III bursts, hence the name ‘reverse’); and (3) an apparent ‘echo’ of the burst some 1 to 2 s later to form a pair. On 1979 February 17/18 a noise storm consisting of Type 1 bursts, Type III bursts and an underlying continuum was observed with the Culgoora spectropolarimeter, spectrograph, and radioheliograph. During this noise storm, the spectrograph record showed several hundred RDP bursts, and about fifty FDPs. Here we report new results on the polarization-of drift pair bursts, present further data on RDP positional and frequency characteristics, and then comment on existing theories concerning RDPs.

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Section: Polarimeter Datasupporting

confidence: 90%

Position and Polarization of Solar Drift Pair Bursts

Suzuki

Gary

1979

Publ. Astron. Soc. Aust.

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“…The motivation for considering the effects of merger on ring galaxies is quite strong, in particular since ring galaxies arise from the most central collisions experienced by disk galaxies. Sastry (1972) and Sastry and AUadin (1977) find in numerical estimates, that head-on collisions between two galaxies will lead to tidal capture if the two galaxies are centrally concentrated (polytropes of index n=4) and collide at relative velocities smaller than 600 km s'^, or to disruption if one is homogeneous and the other is centrally concentrated in a collision with a relative velocity smaller than 500 km S"l. They also find that if the colliding galaxies differ in mass by an order of magnitude, but are of the same dimension, the disruption probability is considerably increased. White (1978), in N-body simulations, finds that in an interpenetrating collisions of two galaxies in bound or parabolic orbits, merger is expected to occur within one initial orbital period.…”

Section: Introductionmentioning

confidence: 99%