Gordeladse, Sh.G. და გორდელაძე, შ. (1938) ახალ ვარსკვლავთა ტემბერატურის შესახებ ანთების საბოლოო ფაზაში / On the Temperature of Novae in the Final Phase of Outburst. აბასთუმნის ასტროფიზიკური ობსერვატორიის ბიულეტენი / Bulletin of the Abastumani Astrophysical Observatory (2). С. 69-97.
|
ტექსტი
1938-10.pdf Download (6MB) | გადახედვა |
რეზიუმე
The present paper deals with the problem of applicability of Zanstra's method for determining the temperature of Novae during the final phase of outburst. As known, in the phase of former Novae acquire the spectrum of Wolf-Rayet stars, whose temperature was also determined by Zanstra's method. This method yields very high temperature values both for Wolf-Rayet stars and for former Novae. It permits to conclude that in the process of outburst the density of Novae increases, since otherwise it would be extremely difficult to explain in what way a star after the outburst acquaires its previous brightness, i.e., the brightness it possessed before the outburst. 1.The total amount of Balmer quanta, formed in the star envelope on account of the energy absorbed by atoms of the envelope, depends not only on the ultraviolet energy of star, absorbed in the envelope beyond the limit of Lyman series, but also on the amount of energy absorbed beyond the limit of Balmer series. 2. The ratio of the quantity of Balmer quanta, formed oil account the energy of stars absorbed beyond the limit of Ba1mer series, to that of Balmer quanta arising from absorption beyond; the limit of Lyman series, depends at the given temperature on the ionization potential and increases with the latter according to the exponential law. In such a way the results yielded by Zanstra's method for former Novae cannot be adopted as reliable. Consequently there are no reasons to consider these stars of being so hot as it is usually surmized. Whence the hypothesis on the increasing density of stars in the process of outburst is rather doubtful. Even in the case the high temperature of these stars were established, this hypothesis would not present the only possible explanation of the in¬crease of temperature, inasmuch as a more natural treating of this problem can be proposed. It is also noteworthy that when studying this problem we have not taken into account one peculiarity, which, no doubt, will take place with moving atoms of large velocities in the case of Wolf-Rayet stars and former Novae. It seems that the differences in frequencies arising at this phenomenon will affect the conditions of radial equilibrium. Therefore at a more rigorous quantitative analysis of the problem one should account for this influence. September, 1937.
| ობიექტის ტიპი: | სტატია |
|---|---|
| თემატიკა: | Q Science > QB Astronomy |
| ქვეგანყოფილება: | Institutes > Evgeny Kharadze Abastumani National Astrophysical Observatory |
| განმათავსებელი მომხმარებელი: | თამარ ჭაღიაშვილი |
| განთავსების თარიღი: | 21 მაისი 2018 10:27 |
| ბოლო ცვლილება: | 02 ივნისი 2018 18:41 |
| URI: | http://eprints.iliauni.edu.ge/id/eprint/7993 |
Actions (login required)
 |
ობიექტის ნახვა |
