Influence of the ionization-energy losses of high-energy bismuth ions on the development of helium blisters in silicon

Within the framework of a semiclassical approximation the general theory of calculation of effective currents and sources generating bremsstrahlung of an arbitrary number of soft quarks and soft gluons at collision of a high-energy color-charged particle with thermal partons in a hot quark–gluon plasma is developed. For the case of one- and two-scattering thermal partons with radiation of one or two soft excitations, the effective currents and sources are calculated in an explicit form. In the model case of "frozen" medium, approximate expressions for energy losses induced by the most simple processes of bremsstrahlung of soft quark and soft gluon are derived. On the basis of a conception of the mutual cancellation of singularities in the sum of so-called "diagonal" and "off-diagonal" contributions to the energy losses, an effective method of determining color factors in scattering probabilities containing the initial values of Grassmann color charges is suggested. The dynamical equations for Grassmann color charges of hard particle used by us earlier on are proved to be insufficient for investigation of the higher radiative processes. It is shown that for correct description of these processes the given equations should be supplemented successively with the higher-order terms in powers of the soft fermionic field.

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BINARY PULSAR SYSTEM PSR B1259-63/LS2883 AS A GAMMA-RAY EMITTER

International Journal of Modern Physics Conference Series ◽

10.1142/s2010194514601690 ◽

2014 ◽

Vol 28 ◽

pp. 1460169 ◽

Cited By ~ 3

Author(s):

DMITRY KHANGULYAN ◽

SERGEY V. BOGOVALOV ◽

FELIX A. AHARONIAN

Keyword(s):

Energy Band ◽

Gamma Ray ◽

High Energy ◽

Energy Losses ◽

Binary Pulsar ◽

Emission Component ◽

Emission Enhancement ◽

Very High Energy ◽

Hydrodynamical Simulations ◽

Very High

Observations of the binary pulsar PSR B1259-63/LS2883 in the high energy and very high energy domains have revealed a few quite unusual features. One of the most puzzling phenomena is the bright GeV flare detected with Fermi/LAT in 2011 January, approximately one month after periastron passage. Since the maximum luminosity in the high energy band during the flare nearly achieved the level of the pulsar spin-down energy losses, it is likely that the particles, responsible for this emission component, had a strongly anisotropic distribution, which resulted in the emission enhancement. One of the most prolific scenarios for such an emission enhancement is the Doppler boosting, which is realized in sources with relativistic motions. Interestingly, a number of hydrodynamical simulations have predicted a formation of highly relativistic outflows in binary pulsar systems, therefore scenarios, involving relativistic boosting, are very natural for these systems. However a more detailed analysis of such a possibility, presented in this study, reveals certain limitations which put strict constraints on the maximum luminosity achievable in this scenario. These constraints render the "Doppler boosting" scenario to be less feasible, especially for the synchrotron models.

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The energy spectrum of the component of the cosmic radiation

Canadian Journal of Physics ◽

10.1139/p68-299 ◽

1968 ◽

Vol 46 (10) ◽

pp. S578-S582 ◽

Cited By ~ 13

Author(s):

P. S. Freier ◽

C. J. Waddington

Keyword(s):

Energy Spectrum ◽

Ionization Energy ◽

Cosmic Radiation ◽

Integral Intensity ◽

Cosmic Ray ◽

Energy Losses ◽

Ionization Energy Loss ◽

Maximum Value ◽

Source Spectra ◽

Acceleration Term

Three large stacks of nuclear emulsions were exposed during 1964–66 on high-altitude balloons launched from Fort Churchill, Canada; Texas, U.S.A.; and Hyderabad, India. These stacks have been used to study the energy spectrum of the cosmic-ray nuclei of calcium and heavier (the so-called VH nuclei). These measurements result in integral intensity values for energies greater than 7.1, 1.58, and 1.00 GeV per nucleon, together with differential intensities over the range [Formula: see text] MeV per nucleon. Differential intensities were also found for lighter nuclei over varying energy ranges. The differential spectrum observed has a maximum value of about 1.6 × 10−3 nuclei/m2 sr s MeV per nucleon around [Formula: see text] MeV per nucleon and falls off at both higher and lower energies. These values are based on the observation of a total of some 1 600 VH nuclei. The energy spectrum has been compared with that observed at similar times for the helium nuclei in order to study the influences of ionization energy losses during propagation of these high-Z nuclei. These observations are interpreted as implying that if the source spectra of the VH nuclei and the helium nuclei are similar, then the VH nuclei have traversed less than 1 g/cm2 of matter while ionization energy loss has been the dominant acceleration term.

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Cosmic ray e± at high energy

EPJ Web of Conferences ◽

10.1051/epjconf/201920804001 ◽

2019 ◽

Vol 208 ◽

pp. 04001 ◽

Cited By ~ 1

Author(s):

Kfir Blum ◽

Annika Reinert

Keyword(s):

Secondary Production ◽

Primary Source ◽

Cosmic Ray ◽

High Energy ◽

Radiative Energy ◽

Energy Losses ◽

Propagation Time ◽

Interstellar Matter ◽

Independent Evidence ◽

Good Agreement

There is a commonly expressed opinion in the literature, that cosmic-ray (CR) e+ come from a primary source, which could be dark matter or pulsars. In these proceedings we review some evidence to the contrary: namely, that e+ come from secondary production due to CR nuclei scattering on interstellar matter. We show that recent measurements of the total e± flux at E ≲ 3 TeV are in good agreement with the predicted flux of secondary e±, that would be obtained if radiative energy losses during CR propagation do not play an important role. If the agreement between data and secondary prediction is not accidental, then the requirement of negligible radiative energy losses implies a very short propagation time for high energy CRs: tesc ≲. 105 yr at rigidities R ≳ 3 TV. Such short propagation history may imply that a recent, near-by source dominates the CRs at these energies. We review independent evidence for a transition in CR propagation, based on the spectral hardening of primary and secondary nuclei around R ~ 100 GV. The transition rigidity of the nuclei matches the rigidity at which the e+ flux saturates its secondary upper bound.

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