一张非常漂亮的天体图--cosmic bird

实际上三个正在并和的星系，看起来像只鸟

Ukwatta 2008 高红移暴的辐射特性

主要内容:
把这些暴的T90, Epeak等画到一张图上。

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文章信息:

· arXiv e-print (arXiv:0802.3815)

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Title:		Screening High-z GRBs with BAT Prompt Emission Properties
Authors:		Ukwatta, T. N.; Sakamoto, T.; Stamatikos, M.; Gehrels, N.; Dhuga, K. S.
Publication:		eprint arXiv:0802.3815
Publication Date:		02/2008
Origin:		ARXIV
Keywords:		Astrophysics
Comment:		4 pages, 4 figures, to be published in the proceedings of ''Gamma Ray Bursts 2007'', Santa Fe, New Mexico, November 5-9
Bibliographic Code:		2008arXiv0802.3815U

Abstract

Detecting high-z GRBs is important for constraining the GRB formation rate, and tracing the history of re-ionization and metallicity of the universe. Based on the current sample of GRBs detected by Swift with known redshifts, we investigated the relationship between red-shift, and spectral and temporal characteristics, using the BAT event-by-event data. We found red-shift trends for the peak-flux-normalized temporal width T90, the light curve variance, the peak flux, and the photon index in simple power-law fit to the BAT event data. We have constructed criteria for screening GRBs with high red-shifts. This will enable us to provide a much faster alert to the GRB community of possible high-z bursts.

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Curran 2008 X射线耀发的统计-和暴本身的flares一脉相承

主要内容:
所以这些flares可能是prelong的或者restarting的central engine。

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文章信息:

· arXiv e-print (arXiv:0802.3803)

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Title:		On the nature of late X-ray flares in Swift Gamma-ray Bursts
Authors:		Curran, P. A.; Starling, R. L. C.; O'Brien, P. T.; Godet, O.; van der Horst, A. J.; Wijers, R. A. M. J.
Publication:		eprint arXiv:0802.3803
Publication Date:		02/2008
Origin:		ARXIV
Keywords:		Astrophysics
Comment:		6 pages, 9 figures, submitted to A&A
Bibliographic Code:		2008arXiv0802.3803C

Abstract

Previously detected in only a few Gamma-ray Bursts (GRBs), X-ray flares are now observed in ~50% of all GRBs, though their origins remain unclear. Most flares are seen early on in the afterglow decay, while some bursts exhibit flares at late times of 10^4 to 10^5 seconds, which may have implications for flare models. We investigate whether a sample of late time (> 10^4 s) flares are different from previous samples of early time flares, or whether they are merely examples on the tail of the early flare distribution. We examine the X-ray light curves of Swift bursts for late flares and compare the flare and underlying power-law properties with those of early flares, and the values of these properties predicted by the blast wave model. The burst sample show late flare properties consistent with those of early flares, where the majority of the flares can be explained by either internal or external shock, though in a few cases one origin is favoured over the other. The underlying power laws are mainly consistent with the normal decay phase of the afterglow. If confirmed by the ever growing sample this would imply that, in some cases, prolonged activity out to late times or a restarting of the central engine is required.

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Butler 2008 GRB统计关系中的选择效应

主要内容:
重点检查了Amati关系E_p-E_iso的选择效应。并说Girlanda关系是没有意义的。

精彩摘抄:
Swift和HETE-II及其他卫星的点在不同的区域

Girlanda关系，黑色的是真实红移，红色的是随机红移，但都不影响关系的致密性，说明关系不依赖于红移，进一步说明关系无意义。

文章信息:

· arXiv e-print (arXiv:0802.3396)

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Title:		Tests for Selection Effects in GRB High-Energy Correlations
Authors:		Butler, Nathaniel R.; Kocevski, Daniel; Bloom, Joshua S.
Publication:		eprint arXiv:0802.3396
Publication Date:		02/2008
Origin:		ARXIV
Keywords:		Astrophysics
Comment:		4 pages, 4 figures, submitted to ApJ
Bibliographic Code:		2008arXiv0802.3396B

Abstract

Several correlations among observables derived from modelling the high-energy properties of GRBs have been reported in the literature. We show that well-known examples of these have common features indicative of an origin in selection effects. In particular, we focus here on the possible origin of the $E_{\rm pk}$-$E_{\rm iso}$ correlation in Swift data due to detector threshold truncation. The existence of faint Swift events calls into question inferences based on pre-Swift surveys which must be subject to complicated incompleteness effects. We review methods for treating data truncation effects in correlation analyses and apply these methods to Swift and pre-Swift data. Also, we show that the $E_{\rm pk}$-$E_{\gamma}$ ("Ghirlanda") correlation is effectively independent of the GRB redshifts, which suggests it contains little intrinsic physics. We recommend verifying that a correlation has significantly reduced scatter in the rest frame relative to the observer frame and also establishing that GRB redshifts contribute meaningfully.

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Brown 2008 UVOT对核坍缩型超新星的观测

主要内容:
包括：
Ib SN2006dn SN2006jc SN2006lt
Ib/c SN2005bf SN2006lc
Ic SN2005da SN2005ek SN2006aj
IIP SN2005cs SN2006at SN2006bc SN2006bp
IIb SN2006T
IIn SN2006bv



精彩摘抄:


文章信息:

· Electronic On-line Article (HTML)

· arXiv e-print (arXiv:0802.3465)

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Title:		Swift UVOT Observations of Core-Collapse SNe
Authors:		Brown, Peter J.; Roming, Peter W. A.; vanden Berk, Daniel E.; Holland, Stephen T.; Immler, Stefan; Milne, Peter
Affiliation:		AA(), AB(), AC(), AD(), AE(), AF()
Publication:		SUPERNOVA 1987A: 20 YEARS AFTER: Supernovae and Gamma-Ray Bursters. AIP Conference Proceedings, Volume 937, pp. 386-390 (2007). (AIPC Homepage)
Publication Date:		10/2007
Origin:		AIP
Keywords:		supernovae, ultraviolet sources (astronomical), red shift, explosions, astronomical telescopes
Abstract Copyright:		(c) 2007: American Institute of Physics
DOI:		10.1063/1.2803595
Bibliographic Code:		2007AIPC..937..386B

Abstract

We review recent UV observations of core-collapse supernovae (SNe) with the Swift Ultra-violet/Optical Telescope (UVOT) during its first two years. Rest-frame UV photometry is useful for differentiating SN types by exploiting the UV-optical spectral shape and more subtle UV features. This is useful for the real-time classification of local and high-redshift SNe using only photometry. Two remarkable SNe Ib/c were observed with UVOT-SN2006jc was a UV bright SN Ib. Swift observations of GRB060218/SN2006aj began shortly after the explosion and show a UV-bright peak followed by a UV-faint SN bump. UV observations are also useful for constraining the temperature and ionization structure of SNe IIP. Rest-frame UV observations of all types are important for understanding the extinction, temperature, and bolometric luminosity of SNe and to interpret the observations of high redshift SNe observed at optical wavelengths.

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Kodama 2008 Yonetoku关系定宇宙学参数

主要内容:
方法回归到典型的定距离的方法：在假定Yonetoku关系正确的基础上，首先用和超新星一样距离的伽玛暴定标，然后延伸到红移大于超新星的地方，得到红移和距离的关系。

精彩摘抄:
距离和红移的关系，蓝色的距离来自超新星，红色的来自Yonetoku关系。

文章信息:

· arXiv e-print (arXiv:0802.3428)

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Title:		Gamma-Ray Bursts in $1.8 <>
Authors:		Kodama, Yoshiki; Yonetoku, Daisuke; Murakami, Toshio; Tanabe, Sachiko; Tsutsui, Ryo; Nakamura, Takashi
Publication:		eprint arXiv:0802.3428
Publication Date:		02/2008
Origin:		ARXIV
Keywords:		Astrophysics
Comment:		4 pages, 4 figures, submitted to MNRAS
Bibliographic Code:		2008arXiv0802.3428K

Abstract

We calibrated the peak energy-peak luminosity relation of GRBs (so called Yonetoku relation) using 33 events with the redshift $z <> Bibtex entry for this abstract Preferred format for this abstract (see Preferences)

Farris 2008 相对论磁流体动力学和辐射的数值模拟

主要内容:
利用广义相对论做3+1的数值模拟，文章给出了数值化的详细的方法。可以作为学习广义相对论数值计算的参考书。

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文章信息:

· arXiv e-print (arXiv:0802.3210)

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Title:		Relativistic Radiation Magnetohydrodynamics in Dynamical Spacetimes: Numerical Methods and Tests
Authors:		Farris, Brian D.; Li, Tsz Ka; Liu, Yuk Tung; Shapiro, Stuart L.
Publication:		eprint arXiv:0802.3210
Publication Date:		02/2008
Origin:		ARXIV
Keywords:		Astrophysics
Comment:		20 pages, 8 figures, submitted to PRD
Bibliographic Code:		2008arXiv0802.3210F

Abstract

Many systems of current interest in relativistic astrophysics require a knowledge of radiative transfer in a magnetized gas flowing in a strongly-curved, dynamical spacetime. Such systems include coalescing compact binaries containing neutron stars or white dwarfs, disks around merging black holes, core collapse supernovae, collapsars, and gamma-ray burst sources. To model these phenomena, all of which involve general relativity, radiation (photon and/or neutrino), and magnetohydrodynamics, we have developed a general relativistic code capable of evolving MHD fluids and radiation in dynamical spacetimes. Our code solves the coupled Einstein-Maxwell-MHD-Radiation system of equations both in axisymmetry and in full 3+1 dimensions. We evolve the metric by integrating the BSSN equations, and use a conservative, high-resolution shock-capturing scheme to evolve both the MHD and radiation moment equations. In this paper, we implement our scheme for optically thick gases and grey-body opacities. Our code gives accurate results in a suite of tests involving radiating shocks and nonlinear waves propagating in Minkowski spacetime. In addition, to test our code's ability to evolve the relativistic radiation-MHD equations in strong-field dynamical spacetimes, we study "thermal Oppenheimer-Snyder collapse" to a black hole, and find good agreement between analytic and numerical solutions.

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Chandra 2008 GRB 070125的观测

主要内容:
给出了这个暴的详细观测数据。

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文章信息:

· arXiv e-print (arXiv:0802.2748)

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Title:		A comprehensive study of GRB 070125, a most energetic gamma ray burst
Authors:		Chandra, Poonam; Cenko, S. Bradley; Frail, Dale; Chevalier, Roger; Macquart, Jean-Pierre; Kulkarni, Shri; Bock, Douglas C. -J.; Bertoldi, Frank; Kasliwal, Mansi; Fox, Derek B.; Price, Paul A.; Berger, Edo; Soderberg, Alicia; Harrison, Fiona A.; Gal-Yam, Avishay; Ofek, Eran; Rau, Arne; Schmidt, Brian P.; Cameron, P. Brian; Cowie, Lennox L.; Cowie, Antoinette; Dopita, Michael; Peterson, Bruce; Penprase, Bryan E.
Publication:		eprint arXiv:0802.2748
Publication Date:		02/2008
Origin:		ARXIV
Keywords:		Astrophysics
Comment:		50 pages, 33 figures, sty file included, Submitted to ApJ on 18th Jan 2008
Bibliographic Code:		2008arXiv0802.2748C

Abstract

We present a comprehensive multiwavelength analysis of the bright, long duration gamma-ray burst GRB 070125, comprised of observations in $\gamma$-ray, X-ray, optical, millimeter and centimeter wavebands. Simultaneous fits to the optical and X-ray light curves favor a break on day 3.78, which we interpret as the jet break from a collimated outflow. Independent fits to optical and X-ray bands give similar results in the optical bands but shift the jet break to around day 10 in the X-ray light curve. We show that for the physical parameters derived for GRB 070125, inverse Compton scattering effects are important throughout the afterglow evolution. While inverse Compton scattering does not affect radio and optical bands, it may be a promising candidate to delay the jet break in the X-ray band. Radio light curves show rapid flux variations, which are interpreted as due to interstellar scintillation, and are used to derive an upper limit of $2.4 \times 10^{17}$ cm on the radius of the fireball in the lateral expansion phase of the jet. Radio light curves and spectra suggest a high synchrotron self absorption frequency indicative of the afterglow shock wave moving in a dense medium. Our broadband modeling favors a constant density profile for the circumburst medium over a wind-like profile ($R^{-2}$). However, keeping in mind the uncertainty of the parameters, it is difficult to unambiguously distinguish between the two density profiles. Our broadband fits suggest that \event is a burst with high radiative efficiency ($> 60 %$).

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Branch 2001 超新星的光学谱

主要内容:
介绍了各类超新星的谱，重点介绍三种拟合谱的程序：SYNOW, NL Monte Carlo, Phoenix。第一个最简单，最后一个最复杂，考虑最齐全。但前者速度快，可以快速变化参数进行拟合。

精彩摘抄:


文章信息:
Optical Spectra of Supernovae

Authors: David Branch, E. Baron, David J. Jeffery

(Submitted on 30 Nov 2001)

Abstract: Supernova flux and polarization spectra bring vital information on the geometry, physical conditions, and composition structure of the ejected matter. For some supernovae the circumstellar matter is also probed by the observed spectra. Some of this information can be inferred directly from the observed line profiles and fluxes, but because of the Doppler broadening and severe line blending, interpretation often involves the use of synthetic spectra. The emphasis in this Chapter is on recent results obtained with the help of synthetic spectra.

Comments:	28 pages, 14 figures, to appear as a Chapter in "Supernovae and Gamma-Ray Bursts", ed. by K. W. Weiler (Springer-Verlag)
Subjects:	Astrophysics (astro-ph)
Cite as:	arXiv:astro-ph/0111573v1

Belmont 2008 一个模拟高能辐射过程的程序

主要内容:
好像还没成熟，值得期待完整的程序。

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文章信息:

· arXiv e-print (arXiv:0802.2661)

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Title:		A new code for radiation processes in high energy plasmas
Authors:		Belmont, R.; Malzac, J.; Marcowith, A.
Publication:		eprint arXiv:0802.2661
Publication Date:		02/2008
Origin:		ARXIV
Keywords:		Astrophysics
Comment:		Poster at the international workshop 'Simbol-X: the hard X-ray universe in focus' held in Bologna, 14-16 May 2007. To appear in Memorie della SAIt, 2 pages, 1 figure
Bibliographic Code:		2008arXiv0802.2661B

Abstract

Extreme objects such as X-ray binaries, AGN, or $\gamma$-ray bursters harbor high energy plasmas whose properties are not well understood yet. Not only are they responsible of the hard X- and $\gamma$-ray emission we observe but also they have a strong influence on the main dynamics and energetics of these objects themselves. Here we present a new kinetic code that solves the evolution equations for particles and photons around compact objects. It produces spectra that will be compared with observations from Simbol-X to constrain the radiation and acceleration processes in these objects.

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Nishikawa 2008 相对论性Particle-In-Cell 模拟伽玛暴瞬时和余辉辐射

主要内容:
模拟显示Webel不稳定性导致了磁场的放大。辐射机制是jitter radiation。
貌似jitter radiation只能数值模拟出来，而不能解析解，所以一般都是做数值计算的文章说，但很有可能就是这种机制，因为同步辐射要求大尺度看随机、小尺度看均匀的磁场，而实际磁场应该更有可能是不均匀并且在时间上也是变化的。

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文章信息:

· arXiv e-print (arXiv:0802.2558)

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Title:		Relativistic Particle-In-Cell Simulation Studies of Prompt and Early Afterglows from GRBs
Authors:		Nishikawa, K. -I.; Hardee, P.; Mizuno, Y.; Medvedev, M.; Zhang, B.; Hartmann, D. H.; Fishiman, G. J.
Publication:		eprint arXiv:0802.2558
Publication Date:		02/2008
Origin:		ARXIV
Keywords:		Astrophysics
Comment:		19 pages,7 figures, contributed talk at Seventh European Workshop on Collisionless Shocks, Paris, 7- 9 November 2007. High resolution version can be obtained at http://gammaray.nsstc.nasa.gov/~nishikawa/shockws07.pdf
Bibliographic Code:		2008arXiv0802.2558N

Abstract

Nonthermal radiation observed from astrophysical systems containing relativistic jets and shocks e.g. gamma-ray bursts (GRBs) active galactic nuclei (AGNs) and microquasars commonly exhibit power-law emission spectra. Recent PIC simulations of relativistic electron-ion (or electron-positron) jets injected into a stationary medium show that particle acceleration occurs within the downstream jet. In collisionless relativistic shocks particle (electron, positron and ion) acceleration is due to plasma waves and their associated instabilities (e.g. the Weibel (filamentation) instability) created in the shock region. The simulations show that the Weibel instability is responsible for generating and amplifying highly non-uniform small-scale magnetic fields. These fields contribute to the electron's transverse deflection behind the jet head. The resulting ``jitter'' radiation from deflected electrons has different properties compared to synchrotron radiation which assumes a uniform magnetic field. Jitter radiation may be important for understanding the complex time evolution and/or spectra in gamma-ray bursts, relativistic jets in general and supernova remnants.

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Kumar 2008 伽玛暴本身的辐射模型

主要内容:
一篇长文章，认为伽玛暴本身的同步辐射模型不能用，暴的时标导致内激波发生的距离很远，远于减速半径了。
认为同步自康普顿可以，参数空间大，还有jitter emission也可能可以，还有电子被持续加热也可能行.

精彩摘抄:


文章信息:

· Electronic On-line Article (HTML)

· Full Printable Article (PDF/Postscript)

· arXiv e-print (arXiv:0802.2704)

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Title:		A general scheme for modeling gamma-ray burst prompt emission
Authors:		Kumar, Pawan; McMahon, Erin; Austin, UT
Publication:		eprint arXiv:0802.2704
Publication Date:		02/2008
Origin:		ARXIV
Keywords:		Astrophysics
Comment:		Published in MNRAS Jan 2008, 56 pages; MNRAS 384, 33, 2008
Bibliographic Code:		2008arXiv0802.2704K

Abstract

We describe a general method for modeling gamma-ray burst prompt emission. We find that for the burst to be produced via the synchrotron process unphysical conditions are required -- the distance of the source from the center of the explosion ($R_\gamma$) must be larger than $\sim 10^{17}$cm and the source Lorentz factor $\gta 10^3$; for such a high Lorentz factor the deceleration radius ($R_d$) is less than $R_\gamma$ even if the number density of particles in the surrounding medium is as small as $\sim 0.1$ cm$^{-3}$. The result, $R_\gamma > R_d$, is in contradiction with the early x-ray and optical afterglow data. The synchrotron-self-Compton (SSC) process fares much better. There is a large solution space for a typical GRB prompt emission to be produced via the SSC process. The prompt optical emission accompanying the burst is found to be very bright ($\lta$ 14 mag; for $z\sim2$) in the SSC model, which exceeds the observed flux (or upper limit) for most GRBs. Continuous acceleration of electrons can significantly reduce the optical flux and bring it down to the observed limits. (Abridged)

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Zhang 2008 自由电子散射对宇宙光子的影响

主要内容:
类似Ia超新星，自由电子的康普顿散射会使得到达观测者的光子数减少。 This Compton dimming increases with redshift and reaches 0.004 mag at $z=1$ and 0.01 mag at $z=2$. 这在宇宙学上可能是需要考虑的现象。

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文章信息:

· arXiv e-print (arXiv:0802.2417)

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Title:		Dimming of supernovae and gamma ray busts by Compton Scattering and its cosmological implications
Authors:		Zhang, Pengjie
Publication:		eprint arXiv:0802.2417
Publication Date:		02/2008
Origin:		ARXIV
Keywords:		Astrophysics
Comment:		3 pages, 3 figures. Submitted to ApJ
Bibliographic Code:		2008arXiv0802.2417Z

Abstract

Free electrons deplete photons from type Ia supernovae through the (inverse) Compton scattering. This Compton dimming increases with redshift and reaches 0.004 mag at $z=1$ and 0.01 mag at $z=2$. Although far from sufficient to invalidate the existence of dark energy, it can bias constraint on dark energy at a level non-negligible for future supernova surveys. This effect is correctable and should be incorporated in supernova analysis. The Compton dimming has similar impact on cosmology based on gamma ray bursts as standard candles.

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Soderberg 2008 XRF 080109/SN 2008D 的X射线和射电观测

主要内容:
数据很全很详细。
投了Nature。

精彩摘抄:
X-ray
radio

文章信息: An Extremely Luminous X-ray Outburst Marking the Birth of a Normal Supernova

Authors: A. M. Soderberg, E. Berger, K. Page, P. Schady, J. Parrent, D. Pooley, X.-Y. Wang, E. Ofek, A. Cucchiara, A. Rau, E. Waxman, J. Simon, D. Bock, P. Milne, M. Page, S. Barthelmy, A. Beardmore, M. Bietenholz, P. Brown, A. Burrows, D. N. Burrows, G. Byrngelson, S. B. Cenko, P. Chandra, J. Cummings, D. B. Fox, A. Gal-Yam, N. Gehrels, S. Immler, M. Kasliwal, A. Kong, H. Krimm, S. R. Kulkarni, P. Meszaros, E. Nakar, P. O'Brien, M. de Pasquale, J. Racusin, N. Rea

(Submitted on 13 Feb 2008)

Abstract: The most massive stars in the universe end their lives in luminous supernova explosions that lead to the formation of neutron stars and black holes and impact star formation and galaxy evolution. For nearly a century, supernovae have been discovered solely through their bright optical emission, delaying initial observations to several days after the explosion. As a result, the details of the core collapse explosion mechanism, as well as the nature of some supernova progenitors, remain a matter of intense debate. Here we report our serendipitous discovery of a normal type Ibc supernova at the time of explosion, marked by an extremely luminous X-ray outburst. We interpret the outburst as the break-out of the supernova shock through a dense wind surrounding the compact (radius of ~10^11 cm) progenitor star. This conclusion is supported by our extensive radio and ultraviolet/optical observations from 0.1 to 30 days post-explosion. Equally important, the inferred rate of X-ray outbursts agrees with the core-collapse supernova rate, leading to the exciting conclusion that future wide-area X-ray surveys will uncover hundreds of supernovae per year at the time of explosion, and thereby enable crucial neutrino and gravitational wave detections that may ultimately unravel the explosion mechanism.

Comments:	Submitted to Nature. 27 pages, 10 figures, supplementary information. Note: this paper has been submitted for publication in Nature and is embargoed for discussion in the press
Subjects:	Astrophysics (astro-ph)
Cite as:	arXiv:0802.1712v1 [astro-ph]

Submission history

From: Alicia Soderberg [view email]
[v1] Wed, 13 Feb 2008 13:10:28 GMT (450kb)

Nomoto 1990 Ic SN 1987M

主要内容:


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文章信息:

· Full Refereed Journal Article (PDF/Postscript)

· Full Refereed Scanned Article (GIF)

· References in the article

· Citations to the Article (41) (Citation History)

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Title:		The type IC supernova 1987M - Core collapse of a low-mass helium star in a binary system
Authors:		Nomoto, K.; Filippenko, A. V.; Shigeyama, T.
Affiliation:		AA(Tokyo, University, Japan; Max-Planck-Institut fuer Physik und Astrophysik, Garching, Federal Republic of Germany), AB(California, University, Berkeley), AC(Tokyo, University, Japan; Max-Planck-Institut fuer Physik und Astrophysik, Garching, Federal Republic of Germany)
Publication:		Astronomy and Astrophysics (ISSN 0004-6361), vol. 240, no. 1, Dec. 1990, p. L1-L4. (A&A Homepage)
Publication Date:		12/1990
Category:		Astrophysics
Origin:		STI
NASA/STI Keywords:		B STARS, BINARY STARS, GRAVITATIONAL COLLAPSE, LIGHT CURVE, SUPERNOVAE, STELLAR EVOLUTION, STELLAR MASS, STELLAR MODELS, STELLAR SPECTROPHOTOMETRY, WOLF-RAYET STARS
Bibliographic Code:		1990A&A...240L...1N

Abstract

Using flux-calibrated spectra, a crude bolometric light curve of the type Ic ('helium-poor Ib') supernova 1987M is constructed. This curve has two important features that are difficult to understand in the context of previous Wolf-Rayet progenitor models: (1) near maximum brightness, SN 1987M was only about 0.5 mag less luminous than type Ia supernovae, significantly brighter than typical type Ib supernovae; and (2) the luminosity of SN 1987M fell more rapidly than that of type Ia and Ib supernovae. A theoretical light curve of an exploding 3.3 solar mass helium star which, in contrast to the previous models, is in good agreement with the observed light curve of SN 1987M is presented. It is shown that SN 1987M may have been the explosion of a helium star of 3-3.5 solar mass that began its life with 12-15 solar mass in a close binary system and gradually lost its mass to the companion.

Swartz 1991 Ic SN 1984L late light curve

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· Full Refereed Journal Article (PDF/Postscript)

· Full Refereed Scanned Article (GIF)

· References in the article

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· NED Objects (10)

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Title:		The late-time light curve of SN 1984L
Authors:		Swartz, Douglas A.; Wheeler, J. C.
Affiliation:		AA(Texas, University, Austin), AB(Texas, University, Austin)
Publication:		Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 379, Sept. 20, 1991, p. L13-L16. Research supported by NSF and Robert A. Welch Foundation. (ApJ Homepage)
Publication Date:		09/1991
Category:		Astrophysics
Origin:		STI
NASA/STI Keywords:		LIGHT CURVE, STELLAR EVOLUTION, SUPERNOVAE, COBALT ISOTOPES, RADIOACTIVE DECAY, STELLAR MASS EJECTION, STELLAR MODELS, STELLAR SPECTRA
DOI:		10.1086/186142
Bibliographic Code:		1991ApJ...379L..13S

Abstract

The V band light curve of the Type Ib supernova SN 1984L indicates that the radioactive cobalt decay products are significantly trapped for times in excess of 400 days. Assuming V is parallel to the bolometric light curve, the observations require on the order of 10 M solar masses of ejecta as shown by expressing the deviation of the bolometric light curve from the cobalt decay curve in terms of the mass, gamma-ray optical depth, and kinetic energy of the ejecta. This result is confirmed by numerical calculations. The large ejecta mass thus deduced is discussed in the context of observations of other Type Ib and Ic supernovae and recent low-mass models of their light curves.

Muller 1992 Ic超新星的高诞生率

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银河系大于1/30yr.

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Title:		High rate for Type IC supernovae
Authors:		Muller, Richard A.; Newberg, Heidi J. M.; Pennypacker, Carlton R.; Perlmutter, Saul; Sasseen, Timothy P.; Smith, Craig K.
Publication:		Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 384, Jan. 1, 1992, p. L9-L13. (ApJ Homepage)
Publication Date:		01/1992
Category:		Astrophysics
Origin:		STI
NASA/STI Keywords:		MILKY WAY GALAXY, SKY SURVEYS (ASTRONOMY), STAR DISTRIBUTION, SUPERNOVAE, REFLECTING TELESCOPES, STELLAR LUMINOSITY
DOI:		10.1086/186251
Bibliographic Code:		1992ApJ...384L...9M

Abstract

Using an automated telescope, 20 SNe in carefully documented observations of nearby galaxies were detected. The SN rates for late spiral (Sbc, Sc, Scd, and Sd) galaxies, normalized to a blue luminosity of 10 exp 10 are 0.4, 1.6, and 1.1 h squared per 100 years for Types Ia, Ic, and II SNe. The rate for Type Ic SNe is significantly higher than found in previous surveys. The rates are not corrected for detection inefficiencies and do not take into account the indications that the Ic SNe are fainter on the average than the previous estimates; therefore the true rates are probably higher. The rates are not strongly dependent on the galaxy inclination, in contradiction to previous compilations. If the Milky Way is a late spiral, then the rate of the Galactic SNe is greater than 1 per 30 +/-7 yr, assuming h = 0.75. This high rate has encouraging consequences for future neutrino and gravitational wave observatories.

van Dyk 1993 Ic SN 1990B radio

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Title:		The radio emission from the type IC supernova SN 1990B
Authors:		van Dyk, Schuyler D.; Sramek, Richard A.; Weiler, Kurt W.; Panagia, Nino
Affiliation:		AA(U.S. Navy, Center for Advanced Space Sensing, Washington), AB(National Radio Astronomy Observatory, Socorro, NM), AC(U.S. Navy, Center for Advanced Space Sensing, Washington), AD(Space Telescope Science Inst., Baltimore, MD)
Publication:		Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 409, no. 1, p. 162-169. (ApJ Homepage)
Publication Date:		05/1993
Category:		Astrophysics
Origin:		STI
NASA/STI Keywords:		RADIO ASTRONOMY, RADIO SOURCES (ASTRONOMY), SUPERNOVAE, VERY LARGE ARRAY (VLA), CALIBRATING, DATA REDUCTION, FLUX DENSITY, LIGHT CURVE
DOI:		10.1086/172652
Bibliographic Code:		1993ApJ...409..162V

Abstract

We present radio observations of the Type Ic SN 1990B in NGC 4568 made with the VLA at 20, 6, 3.6, and 2 cm from 1990 February through 1990 October. We find that its radio properties are quite similar to those of the two previously known Type Ib radio supernovae, SN 1983N and SN 1984L, and clearly distinguishable from the radio emission from Type II radio SNe such as SN 1979C and SN 1986J. Nevertheless, there appear to be smaller, albeit significant, differences in the radio emission and physical properties of Type I from Type Ib radio supernovae. We discuss the radio properties of SN 1990B in the context of progenitor models for the Types Ib/c supernovae and conclude that an interacting binary system origin remains the most promising model. Finally, we suggest that Type Ib, and perhaps Ib/c, radio supernovae may form a class of radio 'standard candles' which could be useful as distance indicators.

Swartz 1993 Ic SN 1987M spectrum

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Title:		Spectra of low-mass helium star models and the type IC supernova SN 1987M
Authors:		Swartz, Douglas A.; Filippenko, Alexei V.; Nomoto, Ken'ichi; Wheeler, J. C.
Affiliation:		AA(Texas Univ., Austin), AB(California Univ., Berkeley), AC(Tokyo Univ., Japan), AD(Texas Univ., Austin)
Publication:		Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 411, no. 1, p. 313-322. (ApJ Homepage)
Publication Date:		07/1993
Category:		Astrophysics
Origin:		STI
NASA/STI Keywords:		B STARS, STELLAR EVOLUTION, STELLAR INTERIORS, STELLAR MASS, STELLAR MODELS, STELLAR SPECTRA, SUPERNOVAE, ATMOSPHERIC MODELS, LIGHT CURVE, STELLAR ATMOSPHERES, VISIBLE SPECTRUM
DOI:		10.1086/172831
Bibliographic Code:		1993ApJ...411..313S

Abstract

The question of whether the low-mass helium star models reproduce the helium-poor Type Ic spectrum of SN 1987M is investigated by comparing the theoretical spectrum from the 3.3-solar-mass model of Shigeyama et al. (1990) to observations of SN 1987M reported by Filippenko et al. (1990). The results indicate a number of positive correlations between the observed and the computed spectra. In both types of spectra, Ca II, O I, and Mg I emission lines dominate at late times, and, if extensive composition mixing is imposed, good fits can be made to the shapes of the emission features and good agreement can be found with the observed ratio of the forbidden and IR triplet blends of Ca II. The former indicates that the 3.3-solar-mass model predicts the proper density/velocity structure, and the latter indicates that the computed temperature structure is consistent with the observation though the lines are too strong relative to the continuum. This result is roughly independent of the He abundance. The computed and observed spectra are consistent with a small Ni-56 production in contrast to Type Ia thermonuclear events whose spectra are dominated by Fe-group lines at late times.

Gomez 1994 Ic SN 1990U 1991A spectra

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Title:		Spectral evolution of the He-Poor supernovae 1990U in NGC 7479 and 1991A in IC 2973
Authors:		Gomez, G.; Lopez, R.
Affiliation:		AA(Instituto de Astrofisica de Carnarias, Tenerife, Spain), AB(Instituto de Astrofisica de Carnarias, Tenerife, Spain)
Publication:		The Astronomical Journal, vol. 108, no. 1, p. 195-201 (AJ Homepage)
Publication Date:		07/1994
Category:		Astrophysics
Origin:		STI
NASA/STI Keywords:		SPECTRUM ANALYSIS, STELLAR EVOLUTION, STELLAR SPECTROPHOTOMETRY, SUPERNOVAE, CHARGE COUPLED DEVICES, STELLAR MASS, STELLAR SPECTRA
DOI:		10.1086/117058
Bibliographic Code:		1994AJ....108..195G

Abstract

We present the spectral evolution, from about one to six months after optical maximum, of two type Ic supernovae, 1990U in NGC 7479 and 1991A in IC 2973 (UGC 6872). We analyze and compare the SN 1990U and SN 1991A spectral sequences. We looked for differences, at similar phases, between the more characteristic spectral features and their evolution. From this analysis, we have found that the overall spectral evolution of these two supernovae followed the same trend. The onset of their nebular phases must have occurred not later than three months after optical maximum. However, we have found some differences between these objects as derived from their spectra. We suggest that SN 1991A was a more oxygen rich and helium poor supernova than SN 1990U.