THE COSMIC RAYS

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THE COSMIC RAYS

• Wolfgang Kundt
• Argelander Institute of Bonn University
• Vulcano, 29 May 2008

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COSMIC-RAY BOOSTING

• Not via multi-step accelerations, (in situ, Fermi
  1, 2 , shock acceleration) Journal of
  Astrophysics and Astronomy 142, 150-156 (1984).
  Note also their highest energies would require
  excessive Bs.
• Rather by single-step sweeping via corotating
  magnetic fields, (eE x B-force) ? see modified
  Hillas plot ? preferentially by magnetars, but
  also by the (coronas of the) central disks of
  active galaxies.

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The SPECTRUM of the COSMIC RAYS

• peaks in power near the ionic rest energy, (a few
  GeV),
• extends in particle energy up towards 1020.5 eV,
• wants Galactic neutron stars as boosters, because
  of
• ?W e (E ? B)dx 1021eV (?
  B)12(?x)6.5 ,
• i.e. via a single fall through a strong
  potential, near the inner edge of a ns
  accretion disk, which will indent deeply into its
  corotating magnetosphere.
• Note that ions above 1018eV are not contained by
  the galaxys magnetic fields (for some 107 yr) ?
  as are the lower-energy ones ? hence abund
  vastly more near their sources. They require
  robust engines.

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THE GAMMA-RAY BURSTS

• Wolfgang Kundt,
• Vulcano, 29 May 2008

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GAMMA-RAY-BURST PROPERTIES
HISTORY

• FIRST DETECTION 2 July 1967
• FIRST CONFERENCE X-mas 1974
• FIRST REPEATER 5 March 1979
• CONSENSUS (1980s) Galactic n
• PRESENT MODELS Fusing binary neutron stars or
  black holes at cosmic
• distances, without further detail
• PREFERRED MODEL as during 80s

Wolfgang Kundt, 27. September 2006
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GAMMA-RAY-BURST PROPERTIES
Burst Spectra
log(? S?)
log(h?/MeV)
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Wolfgang Kundt, 27. September 2006
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GAMMA-RAY-BURST PROPERTIES
CONSTRAINTS (1)

• No Pair Formation at Source d lt kpc /
• Neutron-star Energetics d lt kpc ?
• Afterglow Brightness (at low ?) d lt 0.3 kpc /
• Modest Proper Motion of SGR ( radio lobe) d ?
  30pc
• Tolerable Luminosity of SGR (k-Eddington) d ?
  30pc
• Resolved X-ray Afterglow (growing concentric
  rings)!?
• No Long-Distance travel signatures!? Mitrofanov,
  96
• ? Pre- and Post-cursors (offset by ? hour)!?
  X.Y.Wang P.Mészáros (2007) discuss delays of
  10s and 102s.

Wolfgang Kundt, 27. September 2006
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GAMMA-RAY-BURST PROPERTIES
CONSTRAINTS (2)

• Accreting Galactic dead-pulsar population should
  be
• detected (10-17 M?/yr n) !
• Thin-shell energy distribution ltdmax/dmingt 2 !
• No-Host dilemma Brad Schaefer et al, 97, 99
• Brightness Excess at high z (? 7) B. Schaefer
  07
• Hardness Excess (? 1013 eV) !
• Duration Excess (? hour) !
• Afterglow Brightnesses are z-independent !?
• L(afterglow) ? L(prompt) no beaming ?!

Wolfgang Kundt, 27. September 2006
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CONSTRAINTS (3)
GAMMA-RAY-BURST PROPERTIES

• X-ray Afterglows dont evolve (increasing
  ionization!)
• X-ray Afterglows can fade slowly (? 125 d) !
• All host galaxies when ?, and not fake are
  peculiar, as a class ! B.Cobb Ch.Bailyn
  (2007), also GRB 070125.
• No Orphan Afterglows have been detected !
• Cavallo-Fabian-Rees limit on ?L/?t
• L(after)/L(prompt) ? 1 for GRB 060729 !
• The Mg II absorbers are 4-times overabundant
  (w.r.t. those of quasars), and time-variable
  (hours).
• GRB 070201 has not been seen at g-waves (by
  LIGO).

Wolfgang Kundt, 27. September 2006
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CONSTRAINTS (4)

• Superluminally expanding radio afterglows, like
  for GRB 030329 (41)c, and mystery spots 19c,
  would require pre-existing jet channels G.
  Taylor et al (2005) similarly for SGR 1806-20
  B. Gaensler (2006).
• GRB 080319B was the brightest known optical point
  source in the Universe, aleady 20 sec after
  outburst!
• X-ray afterglow lightcurves show strong flares
  (lt102), between minutes and days after outburst,
  as well as steep falls! Chincarini et al (2007)
  also Troia et al (2007).
• Bright optical afterglow follows ?-ray intensity
  (GRB 080319B) within a few sec, between 13s and
  60s after onset similarly for GRB 990123.

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References

• Aharonian, F., Ozernoy, L., 1979 Astron. Tzirk
  1072, 1
• Chincarini, G., et al (14 authors), 2006, The
  Messenger 123, 54-58
• Colgate, S.A., Petschek, A.G., 1981, Ap. J. 248,
  771-782
• Gehrels, N., et al (20 authors), 2006 Nature
  444, 1044-1046
• Grupe et al, 2007 Ap. J. 662, 443-458
• Hjorth, J., et al (20 authors), 2006 The
  Messenger 126, 16-18
• Kundt, W., 2005 Astrophysics, A New Approach
• Kundt, W., Chang, H.-K., 1993 Astroph. Sp. Sci.
  200, L151-L163
• Marsden, D., Rothschild, R.E., Lingenfelter,
  R.E., 1999 Ap. J. 520, L107-110
• Schaefer, B.E., 1999 Ap.J. 511, L79-L83
• Schaefer, B., 2007 Am.Astr.Soc.Meeting, 12
  highest-z GRBs (52) too bright
• Schmidt, W., 1978 Nature 271, 525-527
• Song, Fu-Gao, Jan. 2008 astro-ph/0801.0780
• Sudilovsky, V., et al (6 authors), 2007 Ap. J.
  669, 741-748
• Taylor,G.B., Frail,D.A., Berger,E.,
  Kulkarni,S.R., 2004 Ap. J. 609, L1-L4
• Vietri, M., Stella, L., Israel, G., 2007
  astro-ph/0702598v1
• Zdziarski, A., 1984 A A 134, 301-305

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PREFERRED MODEL (1)

• Most GRBs come from (ns at distances) d ? (0.1
  , 0.2) kpc.
• The nearest bursts, the SGRs, have distances d
  ? 10 pc.
• The GRBs are emitted by throttled pulsars, whose
  magnetosphere is deeply indented by a low-mass
  accretion disk assembled from its CSM. These
  disks tend to be ? the Milky Way. Their
  (anisotropic) emissions by ricocheting,
  accreting blades peak near their disk plane,
  strengthening an isotropic appearance of the
  bursts in the sky.
• The afterglows are light echos, or transient
  reflection nebulae.
• Centrifugally ejected ion clouds escape
  transluminally, and show up redshifted in
  absorption against the burst impacts light,
  mainly their receding sector. In extreme cases of
  large mass ejections (at small speeds), the
  afterglows can look like SN shells, by acting as
  photon bags.

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PREFERRED MODEL (2)

• The short GRBs, of peak duration lt 2 sec, result
  by accretion of a single blob (blade), of size of
  a terrestrial mountain they are modul- ated by
  the throttled pulsars spin (of period 5s to
  10s), and soften and tail off within some 102
  sec. They form basic events, Piran (2005).
• The long GRBs are superpositions of short GRBs,
  cf. the July 1994 accretion by Jupiter of comet
  Shoemaker-Levy.
• Part of the (hot) accreted blob rises to a large
  scale-height, and gets centrifugally ejected, as
  a transluminal, baryonic burst.
• Occasionally, accretion onto a throttled pulsar
  can trigger additional high-energy activities, of
  much longer duration (than 103 sec).
• SN-like afterglow lightcurves result because of
  SN-like ejections.

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GAMMA-RAY-BURST PROPERTIES

Long
Short
Wolfgang Kundt, 27. September 2006