A new approach to the possibilities of ?(D)-dependence and distances of the supernova remnants

Allakhverdiyev, A. O.; Guseinov, O. H.; Kasumov, F. K.; Yusifov, I. M.

doi:10.1007/bf00648261

Cited by 20 publications

(17 citation statements)

References 27 publications

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“…During this time, Galactic Σ − D relations were studied by Downes (1971), Ilovaisky & Lequeux (1972), Woltjer (1972), Berkhuijsen (1973), Clark & Caswell (1976), Sabbadin (1977), Milne (1979), Caswell & Lerche (1979), Göbel et al (1981), Lozinskaya (1981) and Sakhibov & Smirnov (1982). Critical analysis of this relation began with Allakhverdiyev et al (1983a,b) and continued with the research of Green (1984), Allakhverdiyev et al (1986a), and Allakhverdiyev et al (1986b). Inaccurate calculations of the distances to certain calibrators is the basic deficiency of the relations derived in this manner, i.e.…”

Section: The Galactic Relationmentioning

confidence: 99%

“…Also, the ambient interstellar medium where supernovae explode must be taken into consideration. Allakhverdiyev et al (1983aAllakhverdiyev et al ( , 1983bAllakhverdiyev et al ( , 1986aAllakhverdiyev et al ( , 1986b argued that the Σ − D relation was only applicable to shell-type SNRs. Other significant works on the relation were conducted by Li & Wheeler (1984), Huang & Thaddeus (1985) and Berkhuijsen (1986).…”

Section: The Galactic Relationmentioning

confidence: 99%

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The $\mathsf{\Sigma}$ – Drelation for supernova remnants in nearby galaxies

Urošević

Pannuti

Duric

et al. 2005

A&A

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Abstract. This paper examines relations between the radio surface brightness Σ and the diameter D (also known as Σ − D relations) for a sample of extragalactic supernova remnants (SNRs) as constructed from a combination of published data and data from our own surveys. Our sample of extragalactic SNRs is the largest ever devised for the purpose of analyzing Σ − D relations. The main results of this paper may be summarized as follows: (i) the empirical relations for SNRs in 10 of the 11 nearby galaxies studied have the approximately trivial Σ ∝ D −2 form, therefore limiting their interpretation as physically meaningful relations. In addition, these relations are subject to selection effects rendering them even less useful. Further Monte Carlo simulations suggest that the effect of survey sensitivity has the opposite effect of volume selection (e.g. Malmquist bias, a volume selection effect that shapes the Galactic sample) by tending to flatten the slopes toward a trivial relation. In this case, the true slopes may be steeper than the observed slopes; (ii) compact M 82 SNRs appear to follow a uniquely different Σ− D relation in comparison to the larger, older SNRs in the other 10 galaxies. Monte Carlo simulations suggest that the probability of this difference arising by chance is ≈1% to 10%, depending on what is assumed regarding the underlying SNR population; (iii) three candidate hypernova remnants were identified in our sample of 11 nearby galaxies.

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Section: The Galactic Relationmentioning

confidence: 99%

Section: The Galactic Relationmentioning

confidence: 99%

The $\mathsf{\Sigma}$ – Drelation for supernova remnants in nearby galaxies

Urošević

Pannuti

Duric

et al. 2005

A&A

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“…The reasons for such high dispersions, in other words, the reasons for the Σ-D relation being not very reliable are discussed in detail by Allakhverdiev et al (1986b).…”

Section: Introductionmentioning

confidence: 99%

“…But in most of the cases, as the radiation coming from some parts of the SNR has low intensity the whole of the shell can not be observed (Green's catalog 2001;Caswell & Lerche 1979;Milne 1979;Allakhverdiev et al 1986b). Also in some cases, as the SNR is projected onto a HII region its angular size and its flux can not be measured precisely (Weiler & Panagia 1978;Israel 1980;Blandford & Cowie 1982;Allakhverdiev et al 1983b;Mills et al 1984;Allakhverdiev et al 1986a).…”

Section: Introductionmentioning

confidence: 99%

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The relation between the surface brightness and the diameter for galactic supernova remnants

Guseinov

Ankay

Sezer

et al. 2003

Astronomical & Astrophysical Transactions

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In this work, we have constructed a relation between the surface brightness (Σ) and diameter (D) of Galactic C-and S-type supernova remnants (SNRs). In order to calibrate the Σ-D dependence, we have carefully examined some intrinsic (e.g. explosion energy) and extrinsic (e.g. density of the ambient medium) properties of the remnants and, taking into account also the distance values given in the literature, we have adopted distances for some of the SNRs * huseyin@pascal.sci.akdeniz.edu.tr † askin@gursey.gov.tr ‡ sezer@pascal.sci.akdeniz.edu.tr § physic@lan.ab.az 1 which have relatively more reliable distance values. These calibrator SNRs are all C-and S-type SNRs, i.e. F-type SNRs (and Stype SNR Cas A which has an exceptionally high surface brightness) are excluded. The Sigma-D relation has 2 slopes with a turning point at D=36.5 pc: Σ(at 1 GHz)=8.4 −0.16 Wm −2 Hz −1 ster −1 (for Σ>3.7×10 −21 Wm −2 Hz −1 ster −1 and D<36.5 pc). We discussed the theoretical basis for the Σ-D dependence and particularly the reasons for the change in slope of the relation were stated. Added to this, we have shown the dependence between the radio luminosity and the diameter which seems to have a slope close to zero up to about D=36.5 pc. We have also adopted distance and diameter values for all of the observed Galactic SNRs by examining all the available distance values presented in the literature together with the distances found from our Σ-D relation.

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