scholarly journals Freeze out, IR-catastrophes and Non-thermal Emission in SNe

1996 ◽  
Vol 145 ◽  
pp. 211-222 ◽  
Author(s):  
Claes Fransson ◽  
John Houck ◽  
Cecilia Kozma
Keyword(s):  
Light Curve ◽  
Total Mass ◽  
Thermal Emission ◽  
Sharp Decrease ◽  
Light Curves ◽  
Thermal Excitation ◽  
Sn 1987A ◽  
Ubv Photometry ◽  
Optical Flux ◽  
Freeze Out

Freeze out effects and the IR-catastrophe are discussed for SN 1987A and for Type la SNe. We show that the light curves of the optical lines in SN 1987A provide strong evidence for the IR-catastrophe. We also argue that most optical lines are dominated by non-thermal excitation after ∼ 800 days. The level of this emission is set mainly by the total mass of the elements. Models of the [OI]λλ6300 — 64 light curve show that an oxygen mass of ∼ 1.5Mʘ is needed. Light curve models for Type la SNe display a sharp decrease in the optical flux as a result of the IR-catastrophe at ∼ 500 days, producing UBV-photometry inconsistent with observations of SN1972E by Kirshner & Oke (1975).

scholarly journals The Type II supernovae 2006V and 2006au: two SN 1987A-like events

2011 ◽  
Vol 7 (S279) ◽  
pp. 403-404
Author(s):  
Francesco Taddia
Keyword(s):  
Light Curve ◽  
Near Infrared ◽  
Light Curves ◽  
Type Ii ◽  
Host Galaxies ◽  
Remarkable Similarity ◽  
Sn 1987A ◽  
Nir Light ◽  
Initial Dip ◽  
Analytic Models

AbstractWe studied optical and near-infrared (NIR) light curves, and optical spectra of Supernovae (SNe) 2006V and 2006au, two objects monitored by the Carnegie Supernova Project (CSP) and displaying remarkable similarity to SN 1987A, although they were brighter, bluer and with higher expansion velocities. SN 2006au also shows an initial dip in the light curve, which we have interpreted as the cooling tail of the shock break-out. By fitting semi-analytic models to the UVOIR light curve of each object, we derive the physical properties of the progenitors and we conclude that SNe 2006V and 2006au were most likely Blue Supergiant (BSG) stars that exploded with larger energies as compared to that of SN 1987A. We are currently investigating the host galaxies of a few BSG SNe, in order to understand the role played by the metallicity in the production of these rare exploding BSG stars.

scholarly journals Dust Condensation in the Ejecta of SN 1987A

1989 ◽  
Vol 120 ◽  
pp. 164-179 ◽  
Author(s):  
L.B. Lucy ◽  
I.J. Danziger ◽  
C. Gouiffes ◽  
P. Bouchet
Keyword(s):  
Quantitative Analysis ◽  
Light Curve ◽  
Amorphous Carbon ◽  
Interstellar Dust ◽  
Thermal Emission ◽  
Optical Emission ◽  
Emission Lines ◽  
Carbon Particles ◽  
Sn 1987A ◽  
Dust Condensation

AbstractAn asymmetry of optical emission lines that appeared in Sept. 1988 is interpreted as evidence of dust condensation within the metal-rich ejecta of SN 1987A. A quantitative analysis of this spectroscopic effect is given and shown to be compatible with the photometric record. Moreover, observational and theoretical estimates of the bolometric light curve come into agreement when the far-IR excess is interpreted as thermal emission by grains in the ejecta. A grain population comprising small silicate grains with an admixture of graphite or amorphous carbon particles is suggested by the data. The relevance of this discovery to suggestions that supernovae are major sources of interstellar dust is briefly discussed.

scholarly journals Thermal X-Rays due to Ejecta/CSM Interaction in SN 1987A

1988 ◽  
Vol 108 ◽  
pp. 450-451
Author(s):  
K. Masai ◽  
S. Hayakawa ◽  
H. Itoh ◽  
K. Nomoto ◽  
T. Shigeyama
Keyword(s):  
Light Curve ◽  
Photon Energy ◽  
Thermal Emission ◽  
Circumstellar Matter ◽  
Expansion Velocity ◽  
X Rays ◽  
X Ray ◽  
Sn 1987A ◽  
Inner Radius

The X-ray spectrum observed by Ginga is characterized by a component below 10keV which decreases with increasing photon energy, and a component above 10keV which is nearly flat. This unusual X-ray spectrum may be understood as follows; X-rays below 10keV is likely to be due to thermal emission coming from the shock-heated ejecta, and X-rays above 10keV to be due to γ-ray degradation inside the ejecta. If thermal emission due to the collision of the ejecta with circumstellar matter (CSM) is responsible for X-rays below 10keV, the epoch of the collision can be estimated to be ∼ 0.2yr after the explosion if ∼ 0.5yr is the time when the X-ray flux at ∼ 10keV reaches its maximum. The X-ray light curve then requires the inner radius of CSM to be ∼ 1×1016cm for an expansion velocity, Vex ≃2×109cm s−1.

The freeze-out phase of SN 1987A - Implications for the light curve

1993 ◽  
Vol 408 ◽  
pp. L25 ◽  
Author(s):  
Claes Fransson ◽  
Cecilia Kozma
Keyword(s):  
Light Curve ◽  
Sn 1987A ◽  
Freeze Out

scholarly journals Light Curve Models for SN 1987A and Diagnosis of Supernova Interior

1988 ◽  
Vol 108 ◽  
pp. 319-334
Author(s):  
Ken’ichi Nomoto ◽  
Toshikazu Shigeyama ◽  
Masa-aki Hashimoto
Keyword(s):  
Light Curve ◽  
Reasonable Agreement ◽  
Light Curves ◽  
Shock Propagation ◽  
Helium Abundance ◽  
X Ray ◽  
Sn 1987A ◽  
Shock Heating ◽  
Helium Stars ◽  
Optical Light Curve

AbstractPresupernova evolution of the progenitor of SN 1987A, hydrodynamics of explosion (shock propagation, explosive nucleosynthesis), optical light curve due to shock heating and 56Co decay, and X-ray and γ-ray light curves are calculated and compared with the observations of SN 1987A. Constraints on the mass of the hydrogen-rich envelope Menv (i.e., mass loss history) and the helium abundance in the envelope are obtained from the progenitor’s blue-red-blue evolution as well as from the light curve. The explosion energy E and the mass and distribution of 56Ni are inferred from the light curves. Models and observations are in reasonable agreement for E/Menv = 1.5 ± 0.5 × 1050 erg/M⊙, Menv = 5 - 10 M⊙, and MNi ∼ 0.07 M⊙. Mixing of 56Ni into the envelope is indicated.Light curves of exploding bare helium stars are also calculated to see whether the observed Type Ib supernova light curves can be accounted for.

scholarly journals Systematic study of magnetar-powered hydrogen-rich supernovae

2018 ◽  
Vol 619 ◽  
pp. A145 ◽  
Author(s):  
Mariana Orellana ◽  
Melina C. Bersten ◽  
Takashi J. Moriya
Keyword(s):  
Light Curve ◽  
Light Curves ◽  
Radiation Hydrodynamics ◽  
One Dimensional ◽  
Sn 1987A ◽  
Extra Energy ◽  
Slow Decline ◽  
The Moment ◽  
Rotation Energy ◽  
Equilibrium Radiation

Context. It has been suggested that some supernovae (SNe) may be powered by a magnetar formed at the moment of the explosion. While this scenario has mostly been applied to hydrogen-free events, it may also be possible for hydrogen-rich objects. Aims. We aim to explore the effect of including a magnetar on the light curves of supernovae with H-rich progenitors. Methods. We have applied a version of our one-dimensional local thermodynamic equilibrium radiation hydrodynamics code that takes into account the relativistic motion of the ejecta caused by the extra energy provided by the magnetar. For a fixed red supergiant (RSG) progenitor, we have obtained a set of light curves that corresponds to different values of the magnetar initial rotation energy and the spin-down timescale. The model is applied to SN 2004em and OGLE-2014-SN-073, two peculiar Type II SNe with long-rising SN 1987A-like light curves, although with much larger luminosities. Results. The presence of a plateau phase in either normal or superluminous supernovae is one possible outcome, even if a magnetar is continuously injecting energy into the ejecta. In other cases, the light curve shows a peak but not a plateau. Also, there are intermediate events with a first peak followed by a slow decline and a late break of the declining slope. Our models show that bright and long rising morphologies are possible even assuming RSG structures. Conclusions. A large number of supernova discoveries per year reveal unexpected new types of explosions. According to our results, SLSNe II-P are to be expected, as well as a variety of light curve morphologies that can all be possible signs of a newly born magnetar.

Fast Photometry of the Crab, SN 1987A and Aussat

1989 ◽  
Vol 8 (1) ◽  
pp. 75-77
Author(s):  
K. M. Hill ◽  
A. B. Giles ◽  
R. D. Watson
Keyword(s):  
Specular Reflection ◽  
Light Curves ◽  
Crab Pulsar ◽  
Collection System ◽  
Optical Telescope ◽  
Sn 1987A ◽  
Upper Limits ◽  
Frequency Components ◽  
Optical Flux ◽  
The University

AbstractThe appearance of SN 1987A led to the implementation of a fast sampling option in the data collection system of the photometer on the University of Tasmania’s optical telescope. This option permits acquisition of continuous data trains of over one hour’s duration at sample rates of 5 kHz. Monitoring of SN 1987 A at regular intervals has permitted upper limits to be assigned to any pulsed fraction of the optical flux. Successful test observations of the Crab pulsar have been obtained, as well as observations of the geostationary Aussat satellites during their bi-annual specular-reflection episodes. For the latter, very accurate spin rates (∼1 Hz) are determinable in short data runs because of the higher frequency components (∼100 Hz) in their light curves. These components are produced by the rows of solar cells on the outer surfaces of the satellites, and fast-Fourier transform analyses essentially permit the numbers of rows of cells to be counted precisely.

New Developments in Theoretical Modelling of SN 1987A

1988 ◽  
Vol 7 (4) ◽  
pp. 490-504 ◽  
Author(s):  
Ken’ichi Nomoto ◽  
Toshikazu Shigeyama ◽  
Shiomi Kumagai ◽  
Masa-aki Hashimoto
Keyword(s):  
Light Curve ◽  
Light Curves ◽  
Theoretical Modelling ◽  
New Developments ◽  
X Ray ◽  
The Core ◽  
Sn 1987A ◽  
Recent Developments ◽  
Optical Light Curve ◽  
Nitrogen Abundance

AbstractWe summarise recent developments in modelling SN 1987A including the progenitor’s evolution, explosive nucleosynthesis, optical, X- and γ-ray light curves, and dust formation. The distribution of heavy elements in the ejecta is inferred from the light curves. The pre-peak optical light curve as well as early emergence of X- and γ-ray indicate the mixing of 56Ni into the hydrogen-rich envelope. The plateau-like peak of the optical light curve is well reproduced if hydrogen is mixed into the deep core. The flat X-ray light curve observed by Ginga would be due to the clumpy structure of the core. The progenitor’s blue-red-blue evolution and nitrogen abundance suggest that the progenitor’s hydrogen-rich envelope had mass Menv = 7 − 11 M⊙ and was almost completely mixed.

scholarly journals Three-dimensional mixing and light curves: constraints on the progenitor of supernova 1987A

2019 ◽  
Vol 624 ◽  
pp. A116 ◽  
Author(s):  
V. P. Utrobin ◽  
A. Wongwathanarat ◽  
H.-Th. Janka ◽  
E. Müller ◽  
T. Ertl ◽  
...  
Keyword(s):  
Light Curve ◽  
Maximum Velocity ◽  
Light Curves ◽  
3D Analysis ◽  
Reverse Shock ◽  
Core Mass ◽  
Single Star ◽  
Sn 1987A ◽  
Supernova 1987A ◽  
Larger Sample

With the same method as used previously, we investigate neutrino-driven explosions of a larger sample of blue supergiant models. The blue supergiants were evolved as single-star progenitors. The larger sample includes three new presupernova stars. The results are compared with light-curve observations of the peculiar type IIP supernova 1987A (SN 1987A). The explosions were modeled in 3D with the neutrino-hydrodynamics code PROMETHEUS-HOTB, and light-curve calculations were performed in spherical symmetry with the radiation-hydrodynamics code CRAB, starting at a stage of nearly homologous expansion. Our results confirm the basic findings of the previous work: 3D neutrino-driven explosions with SN 1987A-like energies synthesize an amount of 56Ni that is consistent with the radioactive tail of the light curve. Moreover, the models mix hydrogen inward to minimum velocities below 400 km s−1 as required by spectral observations and a 3D analysis of molecular hydrogen in SN 1987A. Hydrodynamic simulations with the new progenitor models, which possess smaller radii than the older ones, show much better agreement between calculated and observed light curves in the initial luminosity peak and during the first 20 days. A set of explosions with similar energies demonstrated that a high growth factor of Rayleigh–Taylor instabilities at the (C+O)/He composition interface combined with a weak interaction of fast Rayleigh–Taylor plumes, where the reverse shock occurs below the He/H interface, provides a sufficient condition for efficient outward mixing of 56Ni into the hydrogen envelope. This condition is realized to the required extent only in one of the older stellar models, which yielded a maximum velocity of around 3000 km s−1 for the bulk of ejected 56Ni, but failed to reproduce the helium-core mass of 6 M⊙ inferred from the absolute luminosity of the presupernova star. We conclude that none of the single-star progenitor models proposed for SN 1987A to date satisfies all constraints set by observations.

Distance to SN 1987A and the LMC

1999 ◽  
Vol 190 ◽  
pp. 549-554
Author(s):  
Nino Panagia
Keyword(s):  
Angular Size ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Light Curves ◽  
Distance Modulus ◽  
Absolute Size ◽  
Sn 1987A

Using the new reductions of the IUE light curves by Sonneborn et al. (1997) and an extensive set of HST images of SN 1987A we have repeated and improved Panagia et al. (1991) analysis to obtain a better determination of the distance to the supernova. In this way we have derived an absolute size of the ringRabs= (6.23 ± 0.08) x 1017cm and an angular sizeR″ = 808 ± 17 mas, which give a distance to the supernovad(SN1987A) = 51.4 ± 1.2 kpc and a distance modulusm–M(SN1987A) = 18.55 ± 0.05. Allowing for a displacement of SN 1987A position relative to the LMC center, the distance to the barycenter of the Large Magellanic Cloud is also estimated to bed(LMC) = 52.0±1.3 kpc, which corresponds to a distance modulus ofm–M(LMC) = 18.58±0.05.

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