Broad-band non-thermal emission from molecular clouds illuminated by cosmic rays from nearby supernova remnants     

S. Gabici  F. A. Aharonian  S. Casanova 《Monthly notices of the Royal Astronomical Society》2009,396(3):1629-1639

Molecular clouds are expected to emit non-thermal radiation due to cosmic ray interactions in the dense magnetized gas. Such emission is amplified if a cloud is located close to an accelerator of cosmic rays and if energetic particles can leave the accelerator site and diffusively reach the cloud. We consider here a situation in which a molecular cloud is located in the proximity of a supernova remnant which is efficiently accelerating cosmic rays and gradually releasing them in the interstellar medium. We calculate the multiwavelength spectrum from radio to gamma rays which is emerging from the cloud as the result of cosmic ray interactions. The total energy output is dominated by the gamma-ray emission, which can exceed the emission in other bands by an order of magnitude or more. This suggests that some of the unidentified TeV sources detected so far, with no obvious or very weak counterparts in other wavelengths, might be in fact associated with clouds illuminated by cosmic rays coming from a nearby source. Moreover, under certain conditions, the gamma-ray spectrum exhibits a concave shape, being steep at low energies and hard at high energies. This fact might have important implications for the studies of the spectral compatibility of GeV and TeV gamma-ray sources.  相似文献   

Jet and accretion power in the most powerful Fermi blazars     

G. Ghisellini  F. Tavecchio  G. Ghirlanda 《Monthly notices of the Royal Astronomical Society》2009,399(4):2041-2054

Among the blazars detected by the Fermi satellite, we have selected the 23 blazars that in the 3 months of survey had an average γ-ray luminosity above 10⁴⁸ erg s⁻¹. For 17 out of the 23 sources we found and analysed X-ray and optical–ultraviolet data taken by the Swift satellite. With these data, implemented by archival and not simultaneous data, we construct the spectral energy distributions, and interpreted them with a simple one-zone, leptonic, synchrotron and inverse Compton model. When possible, we also compare different high-energy states of single sources, like 0528+134 and 3C 454.3, for which multiple good sets of multiwavelength data are available. In our powerful blazars the high energy emission always dominates the electromagnetic output, and the relatively low level of the synchrotron radiation often does not hide the accretion disc emission. We can then constrain the black hole mass and the disc luminosity. Both are large (i.e. masses equal or greater than  10⁹ M _⊙  and disc luminosities above 10 per cent of Eddington). By modelling the non-thermal continuum we derive the power that the jet carries in the form of bulk motion of particles and fields. On average, the jet power is found to be slightly larger than the disc luminosity, and proportional to the mass accretion rate.  相似文献   

An external-shock origin of the     relation for gamma-ray bursts     

A. Panaitescu 《Monthly notices of the Royal Astronomical Society》2009,393(3):1010-1015

We investigate the possibility that the     relation between the peak energy E _p of the  ν F _ν  spectrum and energy output     for long-duration gamma-ray bursts (GRBs) arises from the external shock produced by the interaction of a relativistic outflow with the ambient medium. To that aim, we take into account the dependence of all parameters which determine E _p and     on the radial distribution of the ambient medium density and find that the     relation can be explained if the medium around GRBs has a universal radial stratification. For various combinations of GRB radiative process (synchrotron or inverse-Compton) and dissipation mechanism (reverse or forward shock), we find that the circumburst medium must have a particle density with a radial distribution different than the   R ⁻²  expected for the stellar wind corresponding to a constant mass-loss rate and terminal speed.  相似文献   

Aspect angle for interstellar magnetic field in SN 1006     

O. Petruk  G. Dubner  G. Castelletti  F. Bocchino  D. Iakubovskyi  M. G. F. Kirsch  M. Miceli  S. Orlando  I. Telezhinsky 《Monthly notices of the Royal Astronomical Society》2009,393(3):1034-1040

A number of important processes taking place around strong shocks in supernova remnants (SNRs) depend on the shock obliquity. The measured synchrotron flux is a function of the aspect angle between interstellar magnetic field (ISMF) and the line of sight. Thus, a model of non-thermal emission from SNRs should account for the orientation of the ambient magnetic field. We develop a new method for the estimation of the aspect angle, based on the comparison between observed and synthesized radio maps of SNRs, making different assumptions about the dependence of electron injection efficiency on the shock obliquity. The method uses the azimuthal profile of radio surface brightness as a probe for orientation of ambient magnetic field because it is almost insensitive to the downstream distribution of magnetic field and emitting electrons. We apply our method to a new radio image of SN 1006 produced on the basis of archival Very Large Array and Parkes data. The image recovers emission from all spatial structures with angular scales from a few arcsec to 15 arcmin. We explore different models of injection efficiency and find the following best-fitting values for the aspect angle of SN 1006:  φ_o= 70^o± 4.2^o  if the injection is isotropic,  φ_o= 64^o± 2.8^o  for quasi-perpendicular injection (SNR has an equatorial belt in both cases) and  φ_o= 11^o± 0.8^o  for quasi-parallel injection (polar-cap model of SNR). In the last case, SN 1006 is expected to have a centrally peaked morphology contrary to what is observed. Therefore, our analysis provides some indication against the quasi-parallel injection model.  相似文献   

Where are Swiftγ-ray bursts beyond the 'synchrotron deathline'?     

V. Savchenko  A. Neronov 《Monthly notices of the Royal Astronomical Society》2009,396(2):935-945

We study time-resolved spectra of the prompt emission of Swift γ-ray bursts (GRB). Our goal is to see if previous BATSE claims of the existence of a large amount of spectra with the low-energy photon indices harder than 2/3 are consistent with Swift data. We perform a systematic search of the episodes of the spectral hardening down to the photon indices  ≤2/3  in the prompt emission spectra of Swift GRBs. We show that the data of the Burst Alert Telescope (BAT) instrument on board of Swift are consistent with BATSE data, if one takes into account differences between the two instruments. Much lower statistics of the very hard spectra in Swift GRBs are explained by the smaller field of view and narrower energy band of the BAT telescope.  相似文献   

Interpretation and implications of the non-detection of GeV spectrum excess by the Fermi Gamma-ray Space Telescope in most gamma-ray bursts     

Yi-Zhong Fan 《Monthly notices of the Royal Astronomical Society》2009,397(3):1539-1548

Since the launch of the Fermi Gamma-ray Space Telescope on 2008 June 11, significant detections of high-energy emission have been reported only in six gamma-ray bursts (GRBs) until now. In this work we show that the lack of detection of a GeV spectrum excess in almost all GRBs, though somewhat surprising, can be well understood within the standard internal shock model and several alternatives like the photosphere internal shock (gradual magnetic dissipation) model and the magnetized internal shock model. The delay of the arrival of the >100 MeV photons from some Fermi bursts can be interpreted too. We then show that with the polarimetry of prompt emission these models may be distinguishable. In the magnetized internal shock model, a high linear polarization level should be typical. In the standard internal shock model, a high linear polarization level is still possible but much less frequent. In the photosphere internal shock model, the linear polarization degree is expected to be roughly anticorrelated with the weight of the photosphere/thermal component, which may be a unique signature of this kind of model. We also briefly discuss the implications of the current Fermi GRB data on the detection prospects of the prompt PeV neutrinos. The influences of the intrinsic proton spectrum and the enhancement of the neutrino number at some specific energies, due to the cooling of pions (muons), are outlined.  相似文献   

Spectral-based k-corrections and implications for the colour–magnitude relation of E/S0s and its evolution     

Nathan Roche  Mariangela Bernardi  Joseph Hyde 《Monthly notices of the Royal Astronomical Society》2009,398(3):1549-1562

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岩体动态应力在地震机理中的作用研究   总被引：4，自引：0，他引：4  

胡志奇  郑文衡  陆明勇 《大地测量与地球动力学》2005,25(1):108-112

根据冲击动力学理论,采用三维动态有限元方法,模拟研究了地壳中的冲击波对地震触发的影响,自然界中随机载荷产生的冲击波导致了库仑应力的减小,引发块体间（或块体内）的错动,因而在地震的触发中,动态应力起很大的作用。  相似文献   

近年首都圈地区中小地震震源机制解及其特征分析   总被引：7，自引：1，他引：6  

兰从欣  邢成起  苗春兰  岳晓媛  郭心  袁学明 《华北地震科学》2005,23(4):21-25

利用Snoke的初动加振幅比方法和59个3分量数字化测震台站记录到的1028条地震波形资料计算了首都圈地区2002～2004年1月41次中小地震的震源机制解,并用随机模型等方法对震源机制解的可靠性做了检验.结果表明该区的震源机制具有一定的区域性特征,如唐山地区以逆断层性质为主,北京-天津地区以正断层性质为主.  相似文献   

化学改性土的工程分类研究   总被引：1，自引：0，他引：1  

姜洪涛  刘瑾  王媛  赵理政 《高校地质学报》2009,15(2)

在已有研究成果和课题组工作的基础上,确立了化学改性土的分类原则,并将其分为5类:即无机类改性土、有机类改性土、无机有机复合类改性土、化学物理类改性土和污染土;给出了各类土的定义,并对它们的成因、工程性质、机理、用途以及优缺点进行了比较详细的分析.研究表明:5类化学改性土具有各自的工程性质特点和形成机理,并适用于不同的工程用途;其改性效果取决于改性材料的性质、被改性土的性质以及改性工艺等,其中化学-物理类改性土的工程性质最具有优势,而污染土一般不能满足工程的环境和强度要求,需要采取一定的措施后,才能作为工程材料使用.化学改性土在环境岩土工程领域中具有广阔的应用前景.  相似文献