Gamma-Ray%20Bursts

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Gamma-Ray Bursts (1) The Pre-BATSE Era
(1967-1991) (2) The BATSE Era The Great
Debate (1991-1997) (3) GRB Intrinsic
Characteristics, Extrinsic Distributions (4) The
Early Afterglow Era (1997-2001) (5) Swift
(2003.?) (6) Short Gamma-Ray Bursts (7) Rapid
Reaction Telescopes
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Scientific Articles 1997 77 1998
161 1999 298
GRBs Intro
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GRB Sky Distribution in Galactic
Coodinates Seven Years of BATSE Observations
Map by Robert Mallozzi
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• HST image GRB 990123 and its host galaxy. The
  scale in this STIS picture is 40 pixels / 1.
• GRB peak luminosity was 2?1053 ergs s-1 ( 1020
  suns, or 109 galaxies).
• GRB brightness at Earth reached 9th magnitude.
  The host galaxy is 24.3 mag.

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• Astronomical magnitude system is logarithmic,
  and arcane
• 1 magnitude ? factor of 2.512 in brightness,
• 5 magnitudes ? factor of 100 in brightness,
  exactly.
• So, (2.512)5 100 .
• 6th magnitude is approximate limit of naked eye
  sensitivity.
• GRB optical counterparts reach 9th to 20th
  magnitude.
• Detected GRB host galaxies are 23rd to 26th
  magnitude,
• 1004 (100 million) ? fainter than naked eye
  sensitivity.

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Selected Length Scales ( ? Niel Brandt
niel_at_ast.cam.ac.uk)   1.44 ? 10-15 meters Rough
nuclear radius 5.3 ? 10-11 meters Hydrogen
atom radius 1.8 meters Humans 8847 meters
Height of Mount Everest 6.3 ? 106 meters Earth
s radius 7.0 ? 108 meters 2 ? 10-8 pc Suns
radius 1.50 ? 1011 meters 5 ? 10-6
pc Earth-to-Sun mean distance (1 Astronomical
Unit 1 AU) 2 ? 1015 meters 0.65 pc ? Oort
Cloud size (Suns Sphere of Influence) 3.08?1016
meters 1 parsec (pc) 3.26 light-years
206,265 AU 4 ? 1016 meters 1.3 pc Sun to
nearest star (Proxima Centauri) 3 ?
1017 meters 10 pc Supernova biological
extinction distance 1.5 ? 1018 meters 50 pc Trigo
nometric parallax distance determination
limit 5.2 ? 1018 meters 170 pc Distance to
supergiant Betelgeuse (supernova in 104 yrs) 1.52
? 1019 meters 500 pc ? Milky Way semi-thickness
( 95 of stars contained) 3.9 ?
1020 meters 13 Kilo pc ? Milky Way disk radius 2
? 1021 meters 65 Kilo pc ? Rough Milky Way dark
matter halo radius 1.9 ? 1022 meters 620 Kilo
pc ? Distance to M31 (Andromeda Nebula) 7 ?
1023 meters 22 Mega pc Distance to center of
Virgo cluster of galaxies 3.0 ?
1025 meters 1 Giga pc ? Luminosity distance to
z0.158 quasar 3C273 1.3 x 1027 meters 5 Giga
pc ? Most distant known quasars Gamma-Ray
Bursters
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Selected Power Scales ( ? Niel Brandt
niel_at_ast.cam.ac.uk)   150 watts Human being
under normal conditions 2 ? 104 watts Car 1 ?
105 watts Running Tyrannosaurus Rex 3 ?
108 watts Nuclear power reactor 3 ?
108 watts Rough thunderstorm electrical power
generation rate 3 ? 1011 watts USA average
electricity usage rate in 1986 8 ?
1013 watts Powerful nanosecond pulse laser 4 ?
1026 watts 1 Lo Solar
luminosity 4 ? 1030 watts 1 ? 104 Lo Cygnus X-1
X-ray luminosity (few solar-mass black hole) 1 ?
1031 watts 3 ? 104 Lo Crab Nebula energy
output 5 ? 1035 watts 1 ? 109 Lo Type II
supernova peak photon luminosity 3 ?
1036 watts 8 ? 109 Lo Milky Way power output 1 ?
1039 watts 4 ? 1011 Lo 108 solar mass accreting
black hole ( quasar luminosity) 4 ?
1032 watts 1 ? 1013 Lo Rough luminosity of
Galactic-halo gamma-ray burst 2 ? 1041 watts 3 ?
1012 Lo Luminosity of z2.286 ultraluminous
galaxy F102144724 1 ? 1042 watts 3 ? 1022
Lo Rough luminosity of cosmological gamma-ray
burst  
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Effects of a Local Gamma-Ray Burst ( burst in
the hood)
The Good News ¾ (Thorset, 1995) Gamma rays alone
will produce ionization in the stratosphere and
create massive amounts of NOx. a catalytic ozone
destroyer
The Bad News ¾ (Shaviv and Dar Model1kpc) TeV
cosmic rays will produce air showers of energetic
muons. At sea level, radiation dosage will be
about 30,000 rads. 100 times the radiation level
lethal to humans
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Ergophobia
2 1033 1021 10-1
2 1053 ergs Msun
c2 e GRB 990123 _at_ z 1.61
E 3 1054 (W/4p) ergs
¼ and the Great Silence ?
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GRBs Lpeak vs. ?
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CCF Lag
Time
GRBs Lpeak vs. ?
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A Main Sequence HR Diagram for Gamma-Ray
Bursts L53 1.1 ? (?lag/0.01 s)-1.15
000131
970228
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Swift Integral Differential , post - Madau
SFR vs. z
GRBs Redshifts
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GRB 970228 z 0.695 Day 200 Rhost 24.6 Scale
1.37/side
GRB 980329 z gt 2 (probable) Day 880 Rhost
28. Galaxy-radio offset 0.75 Scale
17.5/side
GRB 970508 z 0.835 Day 200 Rhost
25.8 Nucleus-OT offset lt 0.01 Scale 9.3 x
10.5
GRB 980519 z unknown Day 750 Rhost
27.5 Galaxy-OT offset 1.5 Scale 6.5/side
GRB 971214 z 3.418 Day 144 Rhost
25.5 Nucleus-OT offset 0.06 Scale
6.35/side
GRB 980613 z 1.097 Day 799 Rhost 26. Field
6 galaxies tidal interactions Scale
18.4/side
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GRB 981226 z 1.097 no OT? Day 555 Rhost
24.3 Nucleus-radio offset 0.7 Scale
2.4/side
GRB 990506 z unknown no OT Day 413 Rhost
25.0 Radio centered on host (fhwm
0.14") Scale 6.3/side
GRB 990123 z 1.600 Day 380 Rhost (3 knots)
28 OT in outer, S. arm Scale 3.2/side
GRB 990510 z 1.619 Day 355 Vhost
28. Nucleus-OT offset 0.066 ( 600 pc) Scale
1.25/side
GRB 990308 z unknown Day 468 Rhosts
27. Galaxy-OT offsets, 1.4 2.2 Scale
6.5/side
GRB 990705 z unknown (low?) Day 387 Vhost
22.8 Nucleus-OT offset 0.9 face-on
spiral Scale 7.6/side
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GRB 990712 z 0.430 Day 287 Rhost 22. OT
centered on bright red knot Scale 1.6/side
GRB 000131 z 4.50 Day 6 RhostOT
24.6 (VLT-Antu 8.2-m) Scale 50/side
GRB 991208 z 0.706 Day 287 Vhost
24.6 Nucleus-OT offset 0.06 Scale
2.5/side
GRB 000301c z 2.03 Day 34 Rhost,OT 26.9,
27.8 Host unresolved Scale 0.9/side
GRB 991216 z 0.77, 0.80, 1.02 Day 123 Rhost
26.9 host diameter, 0.3 BATSE 3rd
ranked Scale 3.2/side
GRB 000418 z 1.118 Day 47 Rhost 23.9 Compact
host (fhwm 0.13") Scale 5/side
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Summary GRB Hosts, SourceHost
Relationship (1) GRB source magnitudes
extrapolated to T0 (R 916) are much brighter
than host galaxy magnitudes (R 2428) ? 104
106 !!! (2) GRB sources are often offset from
nucleus by galactic scale. (3) For
significant fraction ( 1/6), GRB source is
outside but near the (visible portion of) host
galaxy. (4) The galactic scale (FWHM) is often
( 1/3) near HST resolution limit galaxies tend
to be small (1few kpc) at these earlier
epochs. (5) Appearance of interaction, and/or
associated members of a group. (6) Nonzero
probability of incorrect association of GRB
source with a line-of-sight, relatively nearby
(large angular scale) galaxy.
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NFI SRC1
SN1998bw
NFI SRC2
WFC
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GRBs Redshifts
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Motivation. Our understanding of short bursts is
limited to their ?-ray characteristics.
For long bursts, we have multi-? afterglows
yielding redshifts, host galaxies, evidence of
progenitors arising in star-forming regions,
(plus lots of theory ? ).
For short bursts, we have the Small Bump in the
GRB duration plot. In this work, we further
quantify the differences between long and short
GRBs, finding the two classes to have distinct
characteristics.
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gt 100 keV gt 300 keV
0 500 ms
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Akerlof et al.
GRBs Intro
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• Measurement Uncertainties
• Experimental error
• Power law extrapolation
• Bumps and Wiggles
• Range of Optical Magnitudes
• At 10 s 10 16 mags

GRBs Intro