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1.
Valentí Bosch-Ramon 《Astrophysics and Space Science》2007,309(1-4):321-331
Microquasar (MQ) jets are sites of particle acceleration and synchrotron emission. Such synchrotron radiation has been detected
coming from jet regions of different spatial scales, which for the instruments at work nowadays appear as compact radio cores,
slightly resolvedradio jets, or (very) extended structures (e.g. Mirabel and Rodríguez, 1999; Fender, 2001; Corbel et al., 2002). Because of the presence of relativistic particles and dense photon, magnetic and matter fields, these outflows are also
the best candidates to generate the very high-energy (VHE) gamma-rays detected coming from two of these objects, LS 5039 and
LS I +61 303 (Aharonian, 2005; Aharonian et al., 2006a; and Albert, 2006, respectively), and may be contributing significantly to the X-rays emitted from the MQ core (e.g. Markoff et al., 2001; Bosch-Ramon et al., 2005a). In addition, beside electromagnetic radiation, jets at different scales are producing some amount of leptonic and hadronic
cosmic rays (CR), and evidences of neutrino production in these objects may be eventually found. In this work, we review on
the different physical processes that may be at work in or related to MQ jets. The jet regions capable to produce significant
amounts of emission at different wavelengths have been reduced to the jet base, the jet at scales of the order of the size
of the system orbital semi-major axis, the jet middle scales (the resolved radio jets), and the jet termination point. The
surroundings of the jet could be sites of multiwavelength emission as well, deserving also an insight. We focus on those scenarios,
either hadronic or leptonic, in which it seems more plausible to generate both photons from radio to VHE and high-energy neutrinos.
We briefly comment as well on the relevance of MQ as possible contributors to the galactic CR in the GeV–PeV range. 相似文献
2.
Neutrino energy spectra have been calculated based on the recently measured energy spectra of Galactic very high energy γ-ray
sources. Based on these neutrino spectra the expected event rates in the ANTARES neutrino telescope and KM3NeT, a future neutrino
telescope in the Mediterranean Sea with an instrumented volume of one km3, have been calculated. For the brightest γ-ray sources we find event rates of the order of one neutrino per year. Although
the neutrino event rates are comparable to the background from atmospheric neutrinos the detection of individual sources seems
possible. 相似文献
3.
K.N. AbazajianE. Calabrese A. CoorayF. De Bernardis S. Dodelson A. FriedlandG.M. Fuller S. HannestadB.G. Keating E.V. Linder C. LunardiniA. Melchiorri R. Miquel E. PierpaoliJ. Pritchard P. SerraM. Takada Y.Y.Y. Wong 《Astroparticle Physics》2011,35(4):177-184
Cosmological and astrophysical measurements provide powerful constraints on neutrino masses complementary to those from accelerators and reactors. Here we provide a guide to these different probes, for each explaining its physical basis, underlying assumptions, current and future reach. 相似文献
4.
P. A. Sturrock 《Solar physics》2009,254(2):227-239
A search for any particular feature in any single solar neutrino dataset is unlikely to establish variability of the solar
neutrino flux since the count rates are very low. It helps to combine datasets, and in this article we examine data from both
the Homestake and GALLEX experiments. These show evidence of modulation with a frequency of 11.85 year−1, which could be indicative of rotational modulation originating in the solar core. We find that precisely the same frequency
is prominent in power spectrum analyses of the ACRIM irradiance data for both the Homestake and GALLEX time intervals. These
results suggest that the solar core is inhomogeneous and rotates with a sidereal frequency of 12.85 year−1. From Monte Carlo calculations, it is found that the probability that the neutrino data would by chance match the irradiance
data in this way is only 2 parts in 10 000. This rotation rate is significantly lower than that of the inner radiative zone
(13.97 year−1) as recently inferred from analysis of Super-Kamiokande data, suggesting that there may be a second, inner tachocline separating
the core from the radiative zone. This opens up the possibility that there may be an inner dynamo that could produce a strong
internal magnetic field and a second solar cycle. 相似文献
5.
《Astroparticle Physics》2009,32(1):10-41
We present a comprehensive report on the experimental details of the Antarctic Impulsive Transient Antenna (ANITA) long-duration balloon payload, including the design philosophy and realization, physics simulations, performance of the instrument during its first Antarctic flight completed in January of 2007, and expectations for the limiting neutrino detection sensitivity. 相似文献
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8.
Jere H. Jenkins Ephraim Fischbach John B. Buncher John T. Gruenwald Dennis E. Krause Joshua J. Mattes 《Astroparticle Physics》2009,32(1):42-46
Unexplained periodic fluctuations in the decay rates of 32Si and 226Ra have been reported by groups at Brookhaven National Laboratory (32Si), and at the Physikalisch–Technische–Bundesanstalt in Germany (226Ra). We show from an analysis of the raw data in these experiments that the observed fluctuations are strongly correlated in time, not only with each other, but also with the time of year. We discuss both the possibility that these correlations arise from seasonal influences on the detection system, as well as the suggestion of an annual modulation of the decay rates themselves which vary with Earth–Sun distance. 相似文献
9.
D. Horns F. Aharonian A. I. D. Hoffmann A. Santangelo 《Astrophysics and Space Science》2007,309(1-4):189-195
Observations of the inner radian of the Galactic disk at very high energy (VHE) gamma-rays have revealed at least 16 new sources.
Besides shell type super-nova remnants, pulsar wind nebulae (PWN) appear to be a dominant source population in the catalogue
of VHE gamma-ray sources. Except for the Crab nebula, the newly discovered PWN are resolved at VHE gamma-rays to be spatially
extended (5–20 pc). Currently, at least 3 middle aged (t>10 kyrs) PWN (Vela X, G18.0-0.7, and G313.3+0.6 in the “Kookaburra” region) and 1 young PWN MSH 15-52 (t=1.55 kyrs) have been identified to be VHE emitting PWN (sometimes called “TeV Plerions”). Two more candidate “TeV Plerions”
have been identified and have been reported at this conference (Carrigan, These proceedings, in preparation). In this contribution,
the gamma-ray emission from Vela X is explained by a nucleonic component in the pulsar wind. The measured broad band spectral
energy distribution is compared with the expected X-ray emission from primary and secondary electrons. The observed X-ray
emission and TeV emission from the three middle aged PWN are compared with each other. 相似文献
10.
Neutrino production of radio Cherenkov signals in the Moon is the object of radio telescope observations. Depending on the energy range and detection parameters, the dominant contribution to the neutrino signal may come from interactions of the neutrino on the Moon facing the telescope, rather than neutrinos that have traversed a portion of the Moon. Using the approximate analytic expression of the effective lunar aperture from a recent paper by Gayley, Mutel and Jaeger, we evaluate the background from cosmic ray interactions in the lunar regolith. We also consider the modifications to the effective lunar aperture from generic non-standard model neutrino interactions. A background to neutrino signals are radio Cherenkov signals from cosmic ray interactions. For cosmogenic neutrino fluxes, neutrino signals will be difficult to observe because of low neutrino flux at the high energy end and large cosmic ray background in the lower energy range considered here. We show that lunar radio detection of neutrino interactions is best suited to constrain or measure neutrinos from astrophysical sources and probe non-standard neutrino-nucleon interactions such as microscopic black hole production. 相似文献