@article{oai:ir.soken.ac.jp:00003313,
 author = {池内, 了 and IKEUCHI, Satoru},
 journal = {Publications of the Astronomical Society of Japan, Publications of the Astronomical Society of Japan},
 month = {Oct},
 note = {application/pdf, The evolution and structure of two interacting supernova remnants
(SNRS) are calculated by use of a timedependent two-dimensional hydro-
dynamic code. The interactions of two SNRs are simulated in such a
Way that at a time t。 after the first supernova explosion, the second
Supernova explosion occurs at the distance D and two SNRs encounter.
Two cases are investigated; the second explosion occurs outside or in-
Side the expanding she11 0f the first SNR.I n the first case, the final
Structures of two interacting SNRs are typica11y classified into three
types:(1) two SNRs merge into a single-1ike SNR,(2) two SNRs merge
but show a peanut-shape structure, and (3) two SNRs do not merge.1n
the second case, they reduce to two types:(1) Two SNRs evolve as an
isolated SNR with twice the explosion energy, and (2) in the she11 of the
first SNR a bump is formed due to the shock impact by the second ex-
Plosion. The critical distances for the above structural changes are
examined, as we11 as the changes ot the expansion law trom an isolated
SNR. With these results some discussions are given on the formation
of an SNR tunnel system and the possibility of gas ejection from a
galaxy. Based upon this view' of interacting SNRS, a preliminary model
for the solar neighborhood and loop l is presented.},
 pages = {563--580},
 title = {Evolution of Supernova Remnants. 1. Interacting Supernova Remnants},
 volume = {30},
 year = {1978}
}