scholarly journals Using gamma ray monitoring to avoid missing the next Milky Way Type Ia supernova

2019 ◽  
Vol 486 (2) ◽  
pp. 2910-2918 ◽  
Author(s):  
Xilu Wang (王夕露) ◽  
Brian D Fields ◽  
Amy Yarleen Lien (連雅琳)
Keyword(s):  
Gamma Rays ◽  
Milky Way ◽  
Gamma Ray ◽  
Galactic Plane ◽  
Early Warning Systems ◽  
Light Curves ◽  
X Rays ◽  
Warning Systems ◽  
Type Ia Supernova ◽  
Type Ia

Abstract A Milky Way Type Ia supernova (SNIa) could be unidentified or even initially unnoticed, being dim in radio, X-rays, and neutrinos, and suffering large optical/IR extinction in the Galactic plane. But SNIa emit nuclear gamma-ray lines from 56Ni → 56Co → 56Fe radioactive decays. These lines fall within the Fermi/GBM energy range, and the 56Ni 158 keV line is detectable by Swift/BAT. Both instruments frequently monitor the Galactic plane, which is transparent to gamma rays. Thus GBM and BAT are ideal Galactic SNIa early warning systems. We simulate SNIa MeV light curves and spectra to show that GBM and BAT could confirm a Galactic SNIa explosion, followed by Swift localization and observation in X-rays and UVOIR band. The time of detection depends sensitively on the 56Ni distribution, and can be as early as a few days if ${\gtrsim } 10{{\ \rm per\ cent}}$ of the 56Ni is present in the surface as suggested by SN2014J gamma data.

scholarly journals Gamma-Ray Observations of Pulsars

1994 ◽  
Vol 142 ◽  
pp. 789-795
Author(s):  
M. P. Ulmer
Keyword(s):  
Energy Loss ◽  
Gamma Rays ◽  
Gamma Ray ◽  
Rotational Energy ◽  
Light Curves ◽  
Radio Continuum ◽  
X Rays ◽  
X Ray ◽  
Wide Range ◽  
Emission Models

AbstractWe report on Compton Gamma Ray Observatory observations of six detected pulsars: the Crab, Vela, Geminga, PSR B1509-58, PSR B1706-44, and PSR B1055-52. We combine these data with radio data and X-ray data to provide an overview of what is known about gamma-ray pulsars. We discuss light curves, spectra, and radio/gamma-ray phase offsets, and present several tentative patterns in the data. These include constant phase with γ-ray energy; a correlation between gamma-ray and X-ray luminosity; an anticorrelation between the gamma-ray luminosity and the efficiency in converting rotational energy loss into gamma-ray flux; and a correlation between the pulsar period and radio/gamma-ray phase offset. We also suggest that the emission models that have been proposed to date cannot explain the similarities of the average gamma-ray light curves observed over a wide range of energies. Further, unless a narrow beam is assumed, pulsars such as PSR B1055-52 and Geminga appear to be radiating a significant fraction of their rotational energy loss in the form of gamma rays.Subject headings: gamma rays: observations — pulsars: general — radio continuum: stars — X-rays: stars

Hard X‐Rays and Gamma Rays from Type Ia Supernovae

1998 ◽  
Vol 492 (1) ◽  
pp. 228-245 ◽  
Author(s):  
P. Hoflich ◽  
J. C. Wheeler ◽  
A. Khokhlov
Keyword(s):  
Gamma Rays ◽  
Type Ia Supernovae ◽  
X Rays ◽  
Type Ia ◽  
Ia Supernovae

The neutron, gamma-ray, X-ray spectrometer (NGXS): A compact instrument for making combined measurements of neutrons, gamma-rays, and X-rays

2014 ◽  
Vol 93 ◽  
pp. 524-529 ◽  
Author(s):  
David J. Lawrence ◽  
William C. Feldman ◽  
Robert E. Gold ◽  
John O. Goldsten ◽  
Ralph L. McNutt
Keyword(s):  
Gamma Rays ◽  
Gamma Ray ◽  
X Rays ◽  
X Ray ◽  
Combined Measurements

scholarly journals Physical Constraints on Models of Gamma-Ray Bursters

1986 ◽  
Vol 89 ◽  
pp. 305-321
Author(s):  
Richard I. Epstein
Keyword(s):  
Gamma Rays ◽  
Gamma Ray ◽  
High Energy ◽  
X Rays ◽  
Burst Source ◽  
Gamma Ray Burst ◽  
Physical Constraints ◽  
Low Energies ◽  
Energy Gamma ◽  
Photon Interactions

AbstractThe power per logarithmic bandwidth in gamma-ray burst spectra generally increases rapidly with energy through the x-ray range and does not cut off sharply above a few MeV. This spectral form indicates that a very small fraction of the energy from a gamma-ray burst source is emitted at low energies or is reprocessed into x-rays and that the high-energy gamma rays are not destroyed by photon-photon interactions. The implications are that the emission mechanism for the gamma-ray bursts is not synchrotron radiation from electrons that lose most of their energy before being re-accelerated and that either the regions from which the gamma rays are emitted are large compared to the size of a neutron star or the emission is collimated and beamed away from the stellar surface.

scholarly journals The Flare of 1989 September 9, 09:09 UT: Does Coronal Loop Collision Initiate Efficient Gamma-Ray Emission?

1994 ◽  
Vol 142 ◽  
pp. 707-711
Author(s):  
H. Aurass ◽  
A. Hofmann ◽  
E. Rieger
Keyword(s):  
Current Sheet ◽  
Gamma Rays ◽  
Coronal Loop ◽  
Gamma Ray ◽  
High Energy ◽  
X Rays ◽  
Subject Headings ◽  
Γ Ray ◽  
Gamma Ray Emission ◽  
Magnetogram Data

AbstractVector magnetogram data and Hα pictures together with data published by Chupp et al. lead us to conjecture that in the presented case a contact between the rising two-ribbon flare current sheet and a coronal loop connecting two nearby plage regions initiates efficient high-energy γ-ray emission.Subject headings: Sun: corona — Sun: flares — Sun: X-rays, gamma rays

scholarly journals Cosmological Inference from Host-Selected Type Ia Supernova Samples

2017 ◽  
Vol 34 ◽  
Author(s):  
Syed A. Uddin ◽  
Jeremy Mould ◽  
Chris Lidman ◽  
Vanina Ruhlmann-Kleider ◽  
Delphine Hardin
Keyword(s):  
Dark Energy ◽  
Equation Of State ◽  
Real Time ◽  
Matter Density ◽  
Light Curves ◽  
Type Ia Supernova ◽  
Type Ia

AbstractWe compare two Type Ia supernova samples that are drawn from a spectroscopically confirmed Type Ia supernova sample: a host-selected sample in which SNe Ia are restricted to those that have a spectroscopic redshift from the host; and a broader, more traditional sample in which the redshift could come from either the SN or the host. The host-selected sample is representative of SN samples that will use the redshift of the host to infer the SN redshift, long after the SN has faded from view. We find that SNe Ia that are selected on the availability of a redshift from the host differ from SNe Ia that are from the broader sample. The former tend to be redder, have narrower light curves, live in more massive hosts, and tend to be at lower redshifts. We find that constraints on the equation of state of dark energy, w, and the matter density, ΩM, remain consistent between these two types of samples. Our results are important for ongoing and future supernova surveys, which unlike previous supernova surveys, will have limited real-time follow-up to spectroscopically classify the SNe they discover. Most of the redshifts in these surveys will come from the hosts.

THE CASE FOR NON-BARYONIC ENERGY AS THE PRIMARY OUTPUT OF GRBs

2008 ◽  
Vol 17 (09) ◽  
pp. 1333-1341
Author(s):  
D. EICHLER
Keyword(s):  
Kinetic Energy ◽  
Photon Energy ◽  
Radiation Pressure ◽  
Gamma Rays ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Light Curves ◽  
Poynting Flux ◽  
Primary Output ◽  
Primary Form

The evidence is reviewed that the primary form of energy that escapes to infinity from gamma-ray bursts (GRBs) is gamma-rays, and/or Poynting flux, and that the kinetic energy in ultrarelativistic baryons is a secondary component resulting from acceleration of baryons by radiation pressure near or beyond the photosphere. This could account for several observed characteristics of observed GRB spectra and light curves, such as the typical peak photon energy, the correlation of this peak with apparent GRB energy, and the profiles and spectral lagging of GRB subpulses.

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