�ber die Hydrolyse von Anilin

Patat, F.

doi:10.1007/bf00899024

Cited by 97 publications

(144 citation statements)

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“…The shape of the bolometric light curve of model 3F3 is close to the observed bolometric light curve of the`hybrid' SN 1993J, while that of model 3Hb3 recalls the bolometric light curve of SN1987A (Catchpole et al 1987;Hamuy et al 1987), and is also comparable to that of the peculiar SN1909a (see the analysis of Branch 1989, andPatat et al 1994). No observed bolometric light curve has been obtained for the slow SNIc (1962L, 1983V, 1990B and 1990U), but the comparison of the observed B and V light curves (Clocchiatti & Wheeler 1997) with the bolometric light curves corresponding to models 3F3 and 3H3 is interesting.…”

Section: Expansion Of the Envelope And Light Curvessupporting

confidence: 71%

The fate of CO white dwarfs that experience slow deflagrations

Bravo

Domı́nguez

Isern

1999

Monthly Notices of the Royal Astronomical Society

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It has been suggested that the differences among the observational Type Ia supernovae (SNIa) set can be accounted for by invoking two regimes of propagation of combustion. Normal SNIa should be produced by rapid deflagrations that rapidly propagate across a white dwarf, while dim SNIa should be a consequence of a detonation issued during the contraction phase of a pulsation induced by a very slow conductive deflagration. In this paper, we explore the observational consequences of deflagrations, the properties of which are in between both behaviours. Using different laws for the flame velocity as a function of flame radius, a number of different outcomes were found, including direct explosions ejecting small quantities of 56Ni, pulsations leading to recontraction and likely reignition of the flame, and a threshold explosion characterized by an extended gravitationally bound phase (several 103 s), in which most of the white dwarf matter was ejected by the energy input of radioactive isotopes.\ud \ud Not one of these strange supernovae has been detected up to now. Nevertheless, since they are very dim and, for nucleosynthesis reasons, very rare, their existence cannot be excluded. Furthermore, the computed light curve shows that these events mimic the behaviour of peculiar Type II supernovae (SNII), for which reasons there is always the possibility that they have been misclassified as peculiar SNII whose spectrum is lacking.Peer ReviewedPostprint (published version

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Section: Expansion Of the Envelope And Light Curvessupporting

confidence: 71%

The fate of CO white dwarfs that experience slow deflagrations

Bravo

Domı́nguez

Isern

1999

Monthly Notices of the Royal Astronomical Society

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“…The decline rates stated by Sahu et al (2006) from ∼180 to ∼310 d after the explosion in the early nebular phase in B, V, R and I bands are 0.64, 1.04, 1.01 and 1.07 mag, respectively. The flux variation in this phase is marked by the radioactive decay of 56 Co to 56 Fe with an expected decay rate of 0.98 mag/100 d particularly in the V band (Patat et al 1994). Except for the B band, the decline rates during the early nebular phase in V, R and I bands agree fairly well with the expected decay rate of 56 Co to 56 Fe, suggesting that little or no γ -rays escaped during this time.…”

Section: Light Curvesmentioning

confidence: 53%

Type IIP supernova SN 2004et: a multiwavelength study in X-ray, optical and radio

Misra¹,

Pooley²,

Chandra³

et al. 2007

Monthly Notices of the Royal Astronomical Society

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We present X‐ray, broad‐band optical and low‐frequency radio observations of the bright type IIP supernova SN 2004et. The Chandra X‐ray Observatory observed the supernova at three epochs, and the optical coverage spans a period of ∼470 d since explosion. The X‐ray emission softens with time, and we characterize the X‐ray luminosity evolution as LX∝t−0.4. We use the observed X‐ray luminosity to estimate a mass‐loss rate for the progenitor star of ∼2 × 10−6 M⊙ yr−1. The optical light curve shows a pronounced plateau lasting for about 110 d. Temporal evolution of photospheric radius and colour temperature during the plateau phase is determined by making blackbody fits. We estimate the ejected mass of 56Ni to be 0.06 ± 0.03 M⊙. Using the expressions of Litvinova & Nadëzhin we estimate an explosion energy of (0.98 ± 0.25) × 1051 erg. We also present a single epoch radio observation of SN 2004et. We compare this with the predictions of the model proposed by Chevalier, Fransson & Nymark. These multiwavelength studies suggest a main‐sequence progenitor mass of ∼20 M⊙ for SN 2004et.

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“…With the above assumptions for extinction and distance, we obtain M V :217.8<0.3 for the SN absolute magnitude at maximum which, assuming that the (B2V) colour index at maximum is close to zero, is intermediate between the values for 'regular' and bright' SN IIL (respectively 1M B 2:216.8<0.5 and 1M B 2:218.9<0.6; Patat et al 1994).…”

Section: Photometrymentioning

confidence: 84%

“…2, including the discovery estimate by Pollas (1994) and the measurement of Suntzeff (1994). Patat et al (1994) have shown that SN II can be separated on the basis of the parameter 100 , which quantifies the luminosity decline rate in the first 100 d after maximum light. For SN 1994aj we measure B 100 :4.4 mag (100 d) 21 , which is typical of the Linear subclass -very similar, for instance, to SNe 1980K and 1990K.…”

Section: Photometrymentioning

confidence: 99%

Supernova 1994aj: a probe for pre-supernova evolution and mass-loss from the progenitor

Benetti

Danziger

Turatto

et al. 1998

Monthly Notices of the Royal Astronomical Society

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Extensive photometric and spectroscopic observations of SN 1994aj until 540d after maximum light have been obtained. The photometry around maximum suggests that the SN belongs to the Type II Linear class, with a peak absolute magnitude of). The spectra of SN 1994aj were unusual with the presence of a narrow line with a P-Cygni profile on the top of the broad Balmer line emission. This narrow feature is attributed to the presence of a dense superwind surrounding the SN. At 100-120 days after maximum light the SN ejecta starts to interact with this CSM. The SN luminosity decline rates slowed down (γ R = 0.46 mag (100d) −1 ), becoming less steep than the average late luminosity decline of normal SNII (∼ 1 mag (100d) −1 ). This dense (Ṁ /u w ∼ 10 15 g/cm) wind was confined to a short distance from the progenitor (R out =∼ 5 × 10 16 cm), and results from a very strong mass loss episode (Ṁ = 10 −3 M ⊙ /yr), which terminated shortly before explosion (∼ 5 − 10 yr).

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�ber die Hydrolyse von Anilin

Cited by 97 publications

References 0 publications

The fate of CO white dwarfs that experience slow deflagrations

The fate of CO white dwarfs that experience slow deflagrations

Type IIP supernova SN 2004et: a multiwavelength study in X-ray, optical and radio

Supernova 1994aj: a probe for pre-supernova evolution and mass-loss from the progenitor

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