THE COSMIC RAYS Wolfgang Kundt Argelander Institute of

THE COSMIC RAYS Wolfgang Kundt Argelander Institute of Bonn University Vulcano, 29 May 2008

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, (e. E x B-force) see modified Hillas plot preferentially by magnetars, but also by the (coronas of the) central disks of active galaxies.

The SPECTRUM of the COSMIC RAYS • • • peaks in power near the ionic rest energy, (a few Ge. V), extends in particle energy up towards 1020. 5 e. V, wants Galactic neutron stars as boosters, because of: W = e # (E + × B)·dx = 1021 e. V ( × B)12( x)6. 5 , i. e. via a single fall through a strong potential, near the inner edge of a n*´s accretion disk, which will indent deeply into its corotating magnetosphere. • Note that ions above 1018 e. V are not contained by the galaxy´s magnetic fields (for some 107 yr) as are the lower-energy ones hence abund vastly more near their sources. They require robust engines.

THE GAMMA-RAY BURSTS Wolfgang Kundt, Vulcano, 29 May 2008

GAMMA-RAY-BURST PROPERTIES HISTORY • • • FIRST DETECTION: 2 July 1967 FIRST CONFERENCE: X-mas 1974 FIRST REPEATER: 5 March 1979 CONSENSUS (1980 s): Galactic n** PRESENT MODELS: Fusing binary neutron stars or black holes at cosmic distances, without further detail • PREFERRED MODEL: as during 80 s Wolfgang Kundt, 27. September 2006

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

GAMMA-RAY-BURST PROPERTIES CONSTRAINTS (1) • • No Pair Formation at Source: d < kpc / Neutron-star Energetics: d < kpc Afterglow Brightness (at low ): d < 0. 3 kpc / Modest Proper Motion of SGR (& radio lobe): d 30 pc Tolerable Luminosity of SGR (k-Eddington): d 30 pc 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 10 s and 102 s]. Wolfgang Kundt, 27. September 2006

GAMMA-RAY-BURST PROPERTIES CONSTRAINTS (2) • Accreting Galactic dead-pulsar population should be detected (10 -17 M /yr n*) ! • Thin-shell energy distribution: = 2 ! • No-Host dilemma: Brad Schaefer et al, [97, 99] • Brightness Excess at high z ( 7): B. Schaefer [07] • Hardness Excess ( 1013 e. V) ! • Duration Excess ( hour) ! • Afterglow Brightnesses are z-independent !? • L(afterglow) L(prompt): no beaming ? ! Wolfgang Kundt, 27. September 2006

CONSTRAINTS (3) GAMMA-RAY-BURST PROPERTIES • X-ray Afterglows don´t 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

CONSTRAINTS (4) • Superluminally expanding radio afterglows, like for GRB 030329 [(4± 1)c], and mystery spots [19 c], would require pre-existing jet channels [G. Taylor et al (2005)]; similarly for SGR 1806 -20 [B. Gaensler (2006)]. • GRB 080319 B was the brightest known optical point source in the Universe, aleady 20 sec after outburst! • X-ray afterglow lightcurves show strong flares (<102), 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 080319 B) within a few sec, between 13 s and 60 s after onset; similarly for GRB 990123.

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, L 151 -L 163 Marsden, D. , Rothschild, R. E. , Lingenfelter, R. E. , 1999: Ap. J. 520, L 107 -110 Schaefer, B. E. , 1999: Ap. J. 511, L 79 -L 83 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, L 1 -L 4 Vietri, M. , Stella, L. , Israel, G. , 2007: astro-ph/0702598 v 1 Zdziarski, A. , 1984: A & A 134, 301 -305

PREFERRED MODEL (1) • Most GRBs come from (n*s 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 impact´s 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.

PREFERRED MODEL (2) • The short GRBs, of peak duration < 2 sec, result by accretion of a single blob (blade), of size of a terrestrial mountain; they are modul - ated by the throttled pulsar´s spin (of period 5 s to 10 s), 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.

GAMMA-RAY-BURST PROPERTIES Long Short Wolfgang Kundt, 27. September 2006