Analysis of Expansion Processes of a Homogeneous Stellar Gas.

Cernuschi, F.; Marsicano, F. R.

doi:10.1086/109613

Cited by 5 publications

(6 citation statements)

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“…24 The association of interstellar dust and gas had been demonstrated by Bohlin, Savage, & Drake (1978) who found that the color excess and the total hydrogen column density (determined from the observations of HI Lyman-α and H 2 absorption lines with the Copernicus satellite) were well correlated: E(B − V )/N H ≈ 1.7 × 10 −22 mag cm 2 for the diffuse ISM in the solar neighbourhood. This correlation has recently been confirmed by the observations with the Far Ultraviolet Spectroscopic Explorer (FUSE) up to E(B − V ) ≈ 1.0 (Rachford et al 2002), 25 suggesting that the dust and gas are generally well mixed in the ISM. From this ratio of E(B − V ) to N H one can estimate the gas-to-dust mass ratio to be ∼ 210 in the diffuse ISM if we take R V ≈ 3.1 (see Footnote-2 in Li 2004b); together with the "rate of extinction" A V /L ≈ 1.8 mag kpc −1 , one can estimate the hydrogen number density to be n H = R V A V /L N H /E(B − V ) ≈ 1.1 cm −3 and a gas mass density of ρ gas ≈ 2.6 × 10 −24 g cm −3 .…”

Section: Interstellar Grains What Do We Know?mentioning

confidence: 64%

“…Assuming a mean grain size of ∼ 0.1 µm and a typical mass density of ∼ 2.5 g cm −3 for the interstellar grain material, we can estimate the mean dust number density and mass density in the solar neighbourhood ISM respectively to be n dust ≈ 1.1 × 10 −12 cm −3 and ρ dust ≈ 1.2 × 10 −26 g cm −3 from the "rate of extinction". 24 The association of interstellar dust and gas had been demonstrated by Bohlin …”

Section: Interstellar Grains What Do We Know?mentioning

confidence: 87%

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Interstellar grains—the 75th anniversary

2005

J. Phys.: Conf. Ser.

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Section: Interstellar Grains What Do We Know?mentioning

confidence: 64%

Section: Interstellar Grains What Do We Know?mentioning

confidence: 87%

Interstellar grains—the 75th anniversary

2005

J. Phys.: Conf. Ser.

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“…A major goal in the study of CCSNe is to provide a significant test of the proposal that they are, or have been, a significant source of dust in the universe. While this hypothesis is over 30‐yr old (Cernuschi, Marsicano & Codina 1967; Hoyle & Wickramasinghe 1970) and is still popular (Gehrz 1989; Tielens 1990; Dwek 1998; Todini & Ferrara 2001; Nozawa et al 2003) direct evidence that SNe are major dust sources is still very sparse. Indeed, it is not known if ordinary Type II SNe or their progenitors produce large amounts of dust at all.…”

Section: Introductionmentioning

confidence: 99%

Optical and infrared observations of the Type IIP SN 2002hh from days 3 to 397

Pozzo¹,

Meikle²,

Rayner³

et al. 2006

Monthly Notices of the Royal Astronomical Society

131

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We present optical and infrared (IR) observations of the Type II SN 2002hh from 3 to 397 d after explosion. The optical spectroscopic (4-397 d) and photometric (3-278 d) data are complemented by spectroscopic (137-381 d) and photometric (137-314 d) data acquired at IR wavelengths. This is the first time L-band spectra have ever been successfully obtained for a supernova (SN) at a distance beyond the Local Group. The VRI light curves in the first 40 d reveal SN 2002hh to be an SN IIP (plateau) -the most common of all core-collapse SNe. SN 2002hh is one of the most highly extinguished SNe ever investigated. To provide a match between its early-time spectrum and a coeval spectrum of the Type IIP SN 1999em, as well as maintaining consistency with K I interstellar absorption, we invoke a two-component extinction model. One component is due to the combined effect of the interstellar medium (ISM) of our Milky Way Galaxy and the SN host galaxy, while the other component is due to a 'dust pocket' where the grains have a mean size smaller than in the ISM. The early-time optical light curves of SNe 1999em and 2002hh are generally well matched, as are the radioactive tails of these two SNe and SN 1987A. The late-time similarity of the SN 2002hh optical light curves to those of SN 1987A, together with measurements of the optical/IR luminosity and [Fe II] 1.257 μm emission indicate that 0.07 ± 0.02 M of 56 Ni was ejected by SN 2002hh. However, during the nebular phase the HKL luminosities of SN 2002hh exhibit a growing excess with respect to those of SN 1987A. We attribute much of this excess to an IR-echo from a pre-existing, dusty circumstellar medium. Based on an IR-echo interpretation of the near-IR (NIR) excess, we deduce that the progenitor of SN 2002hh underwent recent mass-loss of ∼0.3 M . A detailed comparison of the late-time optical and NIR spectra of SNe 1987A and 2002hh is presented. While the overall impression is one of similarity between the spectra of the two events, there are notable differences. The Mg I 1.503 μm luminosity of SN 2002hh is a factor of 2.5 greater than in SN 1987A at similar epochs, yet coeval silicon and calcium lines in SN 2002hh are fainter. Interpreting these differences as being due to abundance variations, the overall abundance trend between SN 1987A and 2002hh is not consistent with explosion model predictions. It appears that during the burning to intermediate-mass elements, the nucleosynthesis did not progress as far as might have been expected given the mass of iron ejected. Evidence for mixing in the ejecta is presented. Pronounced blueshifts seen in the more isolated lines are attributed to asymmetry in the ejecta. However, during the time-span of these observations (∼1-yr post-explosion) we find no evidence of dust condensation in the ejecta such as might have been revealed by an increasing blueshift and/or attenuation of the red wings of the emission lines. Nevertheless, the clear detection of first overtone CO emission by 200 d and the reddening trend in (K − L ) 0 suggest th...

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“…Already 40 years ago it was suggested that SNe could be an important source of dust in the interstellar medium (Cernuschi, Marsicano & Codina 1967; Hoyle & Wickramasinghe 1970). Recent studies on the origin of dust (Todini & Ferrara 2001; Nozawa et al 2003; Dwek, Galliano & Jones 2007) have supported this view, calling for core‐collapse SNe (CCSNe) as significant sources of dust in the Universe.…”

Section: Dust Formation and Csm Interactionmentioning

confidence: 99%

The Type IIP SN 2007od in UGC 12846: from a bright maximum to dust formation in the nebular phase*

Inserra

Turatto

Pastorello

et al. 2011

Monthly Notices of the Royal Astronomical Society

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Ultraviolet, optical and near‐infrared observations of the Type IIP supernova (SN) 2007od, covering from maximum light to late phases, allow detailed investigation of different physical phenomena in the expanding ejecta. These data turn this object into one of the most peculiar SNe IIP ever studied. The early light curve of SN 2007od is similar to that of a bright IIP, with a short plateau, a bright peak (MV=−18 mag), but a very faint late‐time optical light curve. However, with the inclusion of mid‐IR observations during the radioactive tail, we derive an ejected mass of 56Ni of M(56Ni) ∼2 × 10−2 M⊙. By modelling the bolometric light curve, ejecta expansion velocities and blackbody temperature, we estimate a total ejected mass of 5–7.5 M⊙ with a kinetic energy of at least 0.5 × 1051 erg. The early spectra reveal a boxy Hα profile and high‐velocity features of the Balmer series that suggest the possible interaction of the ejecta with a close circumstellar matter (CSM). The interaction with the CSM and the presence of dust formed inside the ejecta are evident in the late‐time spectra. The episodes of mass‐loss shortly before explosion, the bright plateau, the relatively small amount of 56Ni and the faint [O i] emission observed in the nebular spectra are consistent with a super‐asymptotic giant branch progenitor (M∼ 9.7–11 M⊙).

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Analysis of Expansion Processes of a Homogeneous Stellar Gas.

Cited by 5 publications

References 0 publications

Interstellar grains—the 75th anniversary

Interstellar grains—the 75th anniversary

Optical and infrared observations of the Type IIP SN 2002hh from days 3 to 397

The Type IIP SN 2007od in UGC 12846: from a bright maximum to dust formation in the nebular phase*

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