Review of light curves of novae in the modified scales. II. Classical novae. (arXiv:2007.11025v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Rosenbush_A/0/1/0/all/0/1">A. Rosenbush</a> (Main Astronomical Observatory of NAN of Ukraine)
The presentation of the light curves of the novae on the logarithmic scale of
the radius of the shell ejected during the outburst and in the scale of the
amplitude of the outburst simplified the review of the light curves of all the
known, about 500, classical novae of our Galaxy and the Large and Small
Magellanic Clouds. As a result, the modified light curves about of 250
classical novae were grouped into 7 typical groups with subgroups defined by
the light curves of prototypes. The largest group is the DQ Her group with
V1280 Sco as the main prototype and the key to grouping. Novae of this group
have three or four variants of a dust condensation. Novae of the small GQ Mus
group may be a bright X-ray source during an outburst. CP Pup, CP Lac, V1974
Cyg, and V1493 Aql are prototypes for 4 groups with close tilts of the initial
brightness decline phase of the light curves. The group with RR Pic as
prototype, including the HR Del subgroup, has a prolonged state of maximal
brightness with the presence of several brightness variations before the final
decline phase. The relationship of groups of novae, or form of the light curve,
with processes in the circumstellar and circum-binary system environment is
shortly discussed. The material ejected during an outburst forms expanding
shells of a generally ellipsoidal shape. In the Lac, Pup, and Cyg groups, the
shells do not show a pronounced regular structure, except for their ellipsoidal
shape. Shells of novae with a dust condensation (the DQ Her group) have an
ellipsoidal shape with an equatorial belt. The unique shell of CK Vul, Nova Vul
1670, gives an idea about the possible shape of the shells of other members in
the V1493 Sql group. Each of groups has own position along the well-known
“absolute maximal magnitude, rate of brightness decline” relation.
The presentation of the light curves of the novae on the logarithmic scale of
the radius of the shell ejected during the outburst and in the scale of the
amplitude of the outburst simplified the review of the light curves of all the
known, about 500, classical novae of our Galaxy and the Large and Small
Magellanic Clouds. As a result, the modified light curves about of 250
classical novae were grouped into 7 typical groups with subgroups defined by
the light curves of prototypes. The largest group is the DQ Her group with
V1280 Sco as the main prototype and the key to grouping. Novae of this group
have three or four variants of a dust condensation. Novae of the small GQ Mus
group may be a bright X-ray source during an outburst. CP Pup, CP Lac, V1974
Cyg, and V1493 Aql are prototypes for 4 groups with close tilts of the initial
brightness decline phase of the light curves. The group with RR Pic as
prototype, including the HR Del subgroup, has a prolonged state of maximal
brightness with the presence of several brightness variations before the final
decline phase. The relationship of groups of novae, or form of the light curve,
with processes in the circumstellar and circum-binary system environment is
shortly discussed. The material ejected during an outburst forms expanding
shells of a generally ellipsoidal shape. In the Lac, Pup, and Cyg groups, the
shells do not show a pronounced regular structure, except for their ellipsoidal
shape. Shells of novae with a dust condensation (the DQ Her group) have an
ellipsoidal shape with an equatorial belt. The unique shell of CK Vul, Nova Vul
1670, gives an idea about the possible shape of the shells of other members in
the V1493 Sql group. Each of groups has own position along the well-known
“absolute maximal magnitude, rate of brightness decline” relation.
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