Early spectral evolution  of Nova Sagittarii 2004 (V5114 Sagittarii)

Ederoclite, A.; Mason, E.; Valle, M. Della; Gilmozzi, R.; Williams, Robert E.; Saviane, I.; Matteuccí, F.; Schaefer, Bradley E.; Walter, F.; Rudy, R. J.; Lynch, D. K.; Mazuk, S.; Venturini, C. C.; Puetter, R. C.; Perry, R. B.; Liller, W.; Rotter, A.

doi:10.1051/0004-6361:20065741

Cited by 37 publications

(32 citation statements)

References 21 publications

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“…For example, in the case of Novae the filling factor has been measured to be in the range 10 −2 -10 −5 (Ederoclite et al 2006). Such a filling factor coincides, in our case, with R shell .…”

Section: The Fireshell Fragmentationsupporting

confidence: 75%

GRB 060218 and GRBs associated with supernovae Ib/c

Dainotti¹,

Bernardini²,

Bianco³

et al. 2007

A&A

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Context. The Swift satellite has given continuous data in the range 0.3-150 keV from 0 s to 10 6 s for GRB 060218 associated with SN2006aj. This Gamma-Ray Burst (GRB) which has an unusually long duration (T 90 ∼ 2100 s) fulfills the Amati relation. These data offer the opportunity to probe theoretical models for GRBs connected with Supernovae (SNe). Aims. We plan to fit the complete γ-and X-ray light curves of this long duration GRB, including the prompt emission, in order to clarify the nature of the progenitors and the astrophysical scenario of the class of GRBs associated with SNe Ib/c. Methods. We apply our "fireshell" model based on the formation of a black hole, giving the relevant references. It is characterized by the precise equations of motion and equitemporal surfaces and by the role of thermal emission. Results. The initial total energy of the electron-positron plasma E tot e ± = 2.32 × 10 50 erg has a particularly low value, similar to the other GRBs associated with SNe. For the first time, we observe a baryon loading B = 10 −2 which coincides with the upper limit for the dynamical stability of the fireshell. The effective CircumBurst Medium (CBM) density shows a radial dependence n cbm ∝ r −α with 1.0 < ∼ α < ∼ 1.7 and monotonically decreases from 1 to 10 −6 particles/cm 3 . This behavior is interpreted as being due to a fragmentation in the fireshell. Analogies with the fragmented density and filling factor characterizing Novae are outlined. The fit presented is particularly significant in view of the complete data set available for GRB 060218 and of the fact that it fulfills the Amati relation. Conclusions. We fit GRB 060218, usually considered as an X-Ray Flash (XRF), as a "canonical GRB" within our theoretical model. The smallest possible black hole, formed by the gravitational collapse of a neutron star in a binary system, is consistent with the especially low energetics of the class of GRBs associated with SNe Ib/c. We provide the first evidence for a fragmentation in the fireshell. This fragmentation is crucial in explaining both the unusually large T 90 and the consequently inferred abnormally low value of the CBM effective density.

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Section: The Fireshell Fragmentationsupporting

confidence: 75%

GRB 060218 and GRBs associated with supernovae Ib/c

Dainotti¹,

Bernardini²,

Bianco³

et al. 2007

A&A

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“…The following derivation of the filling factor is laid out according to the following plan: first, we find an analytic expression, in terms of measurables, for the filling factor; then, we detail how we measured the variables and their uncertainty, and then we incorporate the uncertainty into our final calculation. Our method is similar to the one used in Ederoclite et al (2006).…”

Section: Appendix B Deriving the Filling Factormentioning

confidence: 99%

A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date

Finzell

Chomiuk

Metzger

et al. 2018

ApJ

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It has recently been discovered that some, if not all, classical novae emit GeV gamma-rays during outburst, but the mechanisms involved in the production ofgamma-rays are still not well understood. We present here a comprehensive multiwavelength data set-from radio to X-rays-for the most gamma-ray-luminous classical nova to date, V1324 Sco. Using this data set, we show that V1324 Sco is a canonical dusty Fe II-type nova, with a maximum ejecta velocity of 2600 km s −1 and an ejecta mass of a few´-10 5  M . There is also evidence for complex shock interactions, including a double-peaked radio light curve which shows high brightness temperatures at early times. To explore why V1324Sco was so gamma-ray luminous, we present a model of the nova ejecta featuring strong internal shocks and find that higher gamma-ray luminosities result from higher ejecta velocities and/or mass-loss rates. Comparison of V1324Sco with other gamma-ray-detected novae does not show clear signatures of either, and we conclude that a larger sample of similarly well-observed novae is needed to understand the origin and variation of gamma-rays in novae.

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“…As described in Ederoclite et al (2006), the optical depth of λ = 6300 Å line can be calculated from the equation…”

Section: Discussionmentioning

confidence: 99%

On nova Scorpii 2007 N.1 (V1280 Sco)

Kuncarayakti

Kristyowati

Kunjaya

2008

Astrophys Space Sci

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We present the results of our photometric and spectroscopic observations of Nova Sco 2007 N.1 (V1280 Sco). The photometric data was represented by a single data point in the light curve since the observation was carried out only for one night. The spectra cover two different phases of the object's evolution during the outburst, i.e. pre-maximum and post-maximum. Measurements of the P-Cygni profile on Na I 'D' line (5889 Å) was derived as the velocity of shell expansion, yielding 1567.43 ± 174.14 km s −1 . We conclude that V1280 Sco is a fast Fe II-type nova.

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Early spectral evolution of Nova Sagittarii 2004 (V5114 Sagittarii)

Cited by 37 publications

References 21 publications

GRB 060218 and GRBs associated with supernovae Ib/c

GRB 060218 and GRBs associated with supernovae Ib/c

A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date

On nova Scorpii 2007 N.1 (V1280 Sco)

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