Gotowe bibliografie tematyczne / Synchrotron Self Compton (SSC)

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Gotowa bibliografia na temat „Synchrotron Self Compton (SSC)”

Autor: Grafiati

Data publikacji: 6 września 2023

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Artykuły w czasopismach na temat "Synchrotron Self Compton (SSC)"

BÖTTCHER, MARKUS. "MODELING INTERMEDIATE BL LAC OBJECTS DETECTED BY VERITAS". International Journal of Modern Physics D 19, nr 06 (czerwiec 2010): 873–78. http://dx.doi.org/10.1142/s0218271810017135.

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Modeling implications of recent VERITAS discoveries of Intermediate BL Lac Objects (IBLs) are presented. Leptonic jet models for the IBLs W Comae (z = 0.102) and 3C 66A (z = 0.444) are, in principle, viable with only synchrotron and synchrotron self-Compton (SSC) components, but more plausible parameters can be achieved including an external infrared radiation field as source for Compton upscattering to produce the observed VHE gamma-ray emission. The unknown redshift of PKS 1424+240 makes a theoretical interpretation difficult. A pure SSC model seems to be sufficient to represent its SED, and modeling results favor a low redshift of z ≲ 0.1.

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Jacovich, Taylor E., Paz Beniamini i Alexander J. van der Horst. "Modelling synchrotron self-Compton and Klein–Nishina effects in gamma-ray burst afterglows". Monthly Notices of the Royal Astronomical Society 504, nr 1 (6.04.2021): 528–42. http://dx.doi.org/10.1093/mnras/stab911.

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ABSTRACT We present an implementation of a self-consistent way of modelling synchrotron self-Compton (SSC) effects in gamma-ray burst afterglows, with and without approximated Klein–Nishina suppressed scattering for the afterglow modelling code boxfit, which is currently based on pure synchrotron emission. We discuss the changes in spectral shape and evolution due to SSC effects, and comment on how these changes affect physical parameters derived from broad-band modelling. We show that SSC effects can have a profound impact on the shape of the X-ray light curve using simulations including these effects. This leads to data that cannot be simultaneously fit well in both the X-ray and radio bands when considering synchrotron-only fits, and an inability to recover the correct physical parameters, with some fitted parameters deviating orders of magnitude from the simulated input parameters. This may have a significant impact on the physical parameter distributions based on previous broad-band modelling efforts.

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Banasinski, Piotr, i Wlodek Bednarek. "Inhomogeneous SSC model for the γ-ray production in jets of microquasars". Proceedings of the International Astronomical Union 10, S313 (wrzesień 2014): 382–83. http://dx.doi.org/10.1017/s1743921315002537.

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AbstractWe present an inhomogeneous synchrotron self-Compton (SSC) model for active parts of jets in low mass microquasars. We compare results of our model computed, for typical parameters of microquasars, with the sensitivity of Fermi-LAT.

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Yamasaki, Shotaro, i Tsvi Piran. "Analytic modelling of synchrotron self-Compton spectra: Application to GRB 190114C". Monthly Notices of the Royal Astronomical Society 512, nr 2 (25.02.2022): 2142–53. http://dx.doi.org/10.1093/mnras/stac483.

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ABSTRACT Observations of TeV emission from early gamma-ray burst (GRB) afterglows revealed the long sought for inverse Compton (IC) upscattering of the lower energy synchrotron. However, it turned out that the long hoped for ability to easily interpret the synchrotron self-Compton (SSC) spectra didn’t materialize. The TeV emission is in the Klein–Nishina (KN) regime and the simple Thomson regime SSC spectrum is modified, complicating the scene. We describe here a methodology to obtain an analytic approximation to an observed spectrum and infer the conditions at the emitting region. The methodology is general and can be used in any such source. As a test case we apply it to the observations of GRB 190114C. We find that the procedure of fitting the model parameters using the analytic SSC spectrum suffers from some generic problems. However, at the same time, it conveniently gives a useful insight into the conditions that shape the spectrum. Once we introduce a correction to the standard KN approximation, the best-fitting solution is consistent with the one found in detailed numerical simulations. As in the numerical analysis, we find a family of solutions that provide a good approximation to the data and satisfy roughly B ∝ Γ−3 between the magnetic field and the bulk Lorentz factor, and we provide a tentative explanation why such a family arises.

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BANASIŃSKI, PIOTR, i WLODEK BEDNAREK. "THE OPTICALLY THICK HOMOGENEOUS SSC MODEL: APPLICATION TO RADIO GALAXY NGC 1275". International Journal of Modern Physics: Conference Series 28 (styczeń 2014): 1460205. http://dx.doi.org/10.1142/s2010194514602051.

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We consider the Synchrotron Self-Compton (SSC) model for jets in active galaxies in which produced γ-ray photons can be absorbed in collisions with the synchrotron radiation already at the emission region. In terms of such modified SSC model, we argue that the higher emission stages should be characterised by γ-ray spectra extending to lower energies due to the efficient absorption of the highest energy γ-rays. As an example, we show that different emission stages of the nearby radio galaxy NGC 1275 could be explained by such scenario.

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Fedorova, Elena, Bohdan Hnatyk, Antonino Del Popolo, Anatoliy Vasylenko i Vadym Voitsekhovskyi. "Non-Thermal Emission from Radio-Loud AGN Jets: Radio vs. X-rays". Galaxies 10, nr 1 (4.01.2022): 6. http://dx.doi.org/10.3390/galaxies10010006.

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We consider the sample of 55 blazars and Seyferts cross-correlated from the Planck all-sky survey based on the Early Release Compact Source Catalog (ERCSC) and Swift BAT 105-Month Hard X-ray Survey. The radio Planck spectra vs. X-ray Swift/XRT+BAT spectra of the active galactic nuclei (AGN) sample were fitted with the simple and broken power law (for the X-ray spectra taking into account also the Galactic neutral absorption) to test the dependencies between the photon indices of synchrotron emission (in radio range) and synchrotron self-Compton (SSC) or inverse-Compton emission (in X-rays). We show that for the major part of the AGN in our sample there is a correspondence between synchrotron and SSC photon indices (one of two for broken power-law model) compatible within the error levels. For such objects, this can give a good perspective for the task of distinguishing between the jet base counterpart from that one emitted in the disk+corona AGN “central engine”.

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ZACHARIAS, MICHAEL, i REINHARD SCHLICKEISER. "TIME-DEPENDENT SSC COOLING EFFECTS ON BLAZAR EMISSION". International Journal of Modern Physics: Conference Series 28 (styczeń 2014): 1460181. http://dx.doi.org/10.1142/s2010194514601811.

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Blazars are among the most violent sources in the cosmos exhibiting flaring states with remarkably different variability time scales. Especially rapid flares with flux doubling time scales of the order of minutes have been puzzling for quite some time. Many modeling attempts use the well known linear and steady-state scenario for the cooling and emission processes in the jet, albeit the obvious strongly time-dependent nature of flares. Due to the feedback of the self-produced synchrotron radiation with additional scattering by the relativistic electrons, the synchrotron-self Compton (SSC) effect is inherently time-dependent. Recently, an analytical analysis on the effects of this nonlinear behavior has been presented. Here, we summarize these results concerning the effect of the time-dependent SSC cooling on the spectral energy distribution (SED), and the synchrotron lightcurves of blazars. For that, we calculated analytically the synchrotron, SSC and external Compton (EC) component of the SED, giving remarkably different spectral features compared to the standard linear approach. The resulting fluxes strongly depend on the parameters, and SSC might have a strong effect even in sources with strong external photon fields (such as FSRQs). For the synchrotron lightcurve we considered the effects of retardation, including the geometry of the source. The retardation might smear out some effects of the time-dependent cooling, but since lightcurves and SEDs have to be fitted simultaneously with the same set of parameters, the results give nonetheless important clues about the source. Thus, we argue for a wide utilization of the time-dependent treatment in modeling (especially rapid) blazar flares, since it accounts for features in the SED and the lightcurves that are usually accounted for by introducing several breaks in the electron distribution without any physical justification.

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Feng, Yaru, Shaoming Hu, Ruixin Zhou i Songbo Gao. "Explaining the Multiwavelength Emission of γ-ray Bright Flat-Spectrum Radio Quasar 3C 454.3 in Different Activity States". Universe 8, nr 11 (4.11.2022): 585. http://dx.doi.org/10.3390/universe8110585.

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The origin of gamma-ray flares of blazars is still an open issue in jet physics. In this work, we reproduce the multiwavelength spectral energy distribution (SED) of flat-spectrum radio quasars 3C 454.3 under a one-zone leptonic scenario, investigate the variation of the physical parameters in different activity states, and analyze the possible origin of its γ-ray outburst. Based on the analysis of multiwavelength quasi-simultaneous observations of 3C 454.3 during MJD 55,400–56,000, we consider that the radiation includes synchrotron (Syn), synchrotron self-Compton (SSC), and external Compton (EC) radiations by the simulation, and the seed photons of the external Compton component mainly comes from the broad-line region and dusty molecular torus. The model results show that: (1) We can well reproduce the multiwavelength quasi-simultaneity SED of 3C 454.3 in various activity states by using a one-zone Syn+SSC+EC model. (2) By comparing the physical model parameters of the bright and the quiescent states, we suggest that this γ-ray flaring activity is more likely to be caused by the increase in the doppler factor.

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Fraija, N., M. G. Dainotti, Sahil Ugale, Debarpita Jyoti i Donald C. Warren. "Synchrotron Self-Compton Afterglow Closure Relations and Fermi-LAT-detected Gamma-Ray Bursts". Astrophysical Journal 934, nr 2 (1.08.2022): 188. http://dx.doi.org/10.3847/1538-4357/ac7a9c.

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Abstract The Fermi Large Area Telescope (Fermi-LAT) Collaboration reported the Second Gamma-ray Burst Catalog (2FLGC), which comprises a subset of 29 bursts with photon energies above 10 GeV. Although the standard synchrotron forward-shock model has successfully explained the gamma-ray burst (GRB) afterglow observations, energetic photons higher than 10 GeV from these transient events can hardly be described in this scenario. We present the closure relations (CRs) of the synchrotron self-Compton (SSC) afterglow model in the adiabatic and radiative scenario, and when the central engine injects continuous energy into the blast wave to study the evolution of the spectral and temporal indexes of those bursts reported in 2FLGC. We consider the SSC afterglow model evolving in stellar-wind and the interstellar medium (ISM), and the CRs as a function of the radiative parameter, the energy injection index, and the electron spectral index for 1 < p < 2 and 2 ≤ p. We select all GRBs that have been modeled with both a simple or a broken power law in the 2FLGC. We found that the CRs of the SSC model can satisfy a significant fraction of the burst that cannot be interpreted in the synchrotron scenario, even though those that require an intermediate density profile (e.g., GRB 130427A) or an atypical fraction of total energy given to amplify the magnetic field (ε B ). The value of this parameter in the SSC model ranges (ε B ≈ 10−5 − 10−4) when the cooling spectral break corresponds to the Fermi-LAT band for typical values of GRB afterglow. The analysis shows that the ISM is preferred for the scenario without energy injection and the stellar-wind medium for an energy injection scenario.

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Joshi, Jagdish C., i Soebur Razzaque. "Modelling synchrotron and synchrotron self-Compton emission of gamma-ray burst afterglows from radio to very-high energies". Monthly Notices of the Royal Astronomical Society 505, nr 2 (10.05.2021): 1718–29. http://dx.doi.org/10.1093/mnras/stab1329.

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ABSTRACT Synchrotron radiation from a decelerating blastwave is a widely accepted model of radio to X-ray afterglow emission from gamma-ray bursts (GRBs). GeV gamma-ray emission detected by the Fermi Large Area Telescope (LAT) and the duration of which extends beyond the prompt gamma-ray emission phase is also compatible with broad features of afterglow emission. We revisit the synchrotron self-Compton (SSC) emission model from a decelerating blastwave to fit multiwavelength data from three bright GRBs, namely GRB 190114C, GRB 130427A, and GRB 090510. We constrain the afterglow model parameters using the simultaneous fit of the spectral energy distributions at different times and light curves at different frequencies for these bursts. We find that a constant density interstellar medium is favoured for the short GRB 090510, while a wind-type environment is favoured for the long GRB 130427A and GRB 190114C. The sub-TeV component in GRB 190114C detected by MAGIC is the SSC emission in our modelling. Furthermore, we find that the SSC emission in the Thomson regime is adequate to fit the spectra and light curves of GRB 190114C. For the other two GRBs, lacking sub-TeV detection, the SSC emissions are also modelled in the Thomson regime. For the model parameters we have used, the γγ attenuation in the blastwave is negligible in the sub-TeV range compared to the redshift-dependent γγ attenuation in the extragalactic background light.

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Rozprawy doktorskie na temat "Synchrotron Self Compton (SSC)"

Sanchez, David. "Étude et modélisation des noyaux actifs de galaxie les plus énergétiques avec le satellite Fermi". Phd thesis, Ecole Polytechnique X, 2010. http://pastel.archives-ouvertes.fr/pastel-00521741.

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Lancé le 11 juin 2008 par la NASA, le satellite \textit{Fermi}, avec à son bord le LAT (Large Area Telescope), ouvre une nouvelle fenêtre sur le ciel gamma. Grâce à aux capacités de détection du LAT des photons dans la gamme en énergie 200 MeV-300 GeV, il devient possible d'étudier les Noyaux Actifs de Galaxie (NAG en anglais). En particulier, on s'intéressera à la classe des blazars et les plus énergétiques d'entres-eux les High frequency peaked BL Lac (HBL). Les blazars sont des NAG possédant un jet qui pointe dans la direction de la Terre. Cette thèse présente une étude systématique des blazars détectés par les observatoires Tcherenkov au dessus de 200 GeV, faite avec 5.5 mois de données prisent par le LAT. La comparaison entre les deux gammes en énergie permet d'étudier la distribution des particules émettrices ainsi que des effets de propagation des photons de la source jusqu'à l'observateur. Un modèle d'émission électromagnétique des jets de plasma dit synchrotron self-Compton (SSC) est décrit et utilisé pour rendre compte de l'émission sur tout le spectre des HBL PKS 2155-305 et PG 1553+113. Les résultats indiquent que les effets Klein-Nishina de réduction de la section efficace de diffusion Compton inverse jouent un rôle majeur dans ces objets. Une étude sur le long terme (environ 1 an) de PKS 2155-305 en rayons X et en rayons gamma est aussi décrite. Menée avec le satellite RXTE (rayons X) et le LAT, c'est la campagne d'observation conjointe la plus longue à ce jour. Les propriétés spectrales et temporelles sont décrites avec un modèle SSC dépendant du temps.

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Celotti, Anna Lisa. "The Role of Synchrotron and Self Compton Radiation in Active Galactic Nuclei". Doctoral thesis, SISSA, 1992. http://hdl.handle.net/20.500.11767/4215.

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Lucertini, Francesca. "Emissione di Compton inverso e applicazioni astrofisiche". Bachelor's thesis, Alma Mater Studiorum - Università di Bologna, 2015. http://amslaurea.unibo.it/8869/.

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Con questa Tesi si vuole illustrare L'effetto Compton inverso e alcune delle sue applicazioni astrofisiche. Poichè l'effetto Compton inverso è un processo di scattering si è ritenuto importante spiegare, brevemente, la diffusione Thomson e la diffusione Compton per mostrare le differenze tra i tre processi. Successivamente si è studiata l'emissione per Compton inverso dovuta a una singola interazione, la potenza e lo spettro del caso generale. Tra le applicazioni astrofisiche si sono riportate la Comptonizzazione e il Synchrotron self-Compton, per poi approfondire ognuna con una esempio specifico. Nel caso della Comptonizzazione si è discusso l'effetto Sunyaev-zeldovich mentre i BL Lacertae rappresentano l'approfondimento relatico al Synchrotron self-Compton.

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Ohlsson, Pierre. "Gamma-ray emission and Synchrotron Self-Compton modelling of the macrolensed Quasar PKS 1830-211". Thesis, Linnéuniversitetet, Institutionen för fysik och elektroteknik (IFE), 2020. http://urn.kb.se/resolve?urn=urn:nbn:se:lnu:diva-107138.

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The objective of this thesis is to retrieve Light Curves, Spectral Models, Spectral Maps, and to geta Spectral Energy Distribution (SED) plot, for the source of PKS1830-211. Finally, also to do amodelling of the whole SED coming from the source with the JetSet software. Which will then becompared to a previous modelling done by A. A. Abdo. First, a light curve is taken over the wholeFermi duration period. The Light Curve is a statistical plot of the overall flux from the source overtime. It will set every photon in a defined energy interval as a datapoint in a defined time bin width. Alight curve will first be taken over the Fermi Duration Period, to get a view of potential flares comingfrom the source. Three periods are then chosen to get a loud, an intermediate, and a loud flaringperiod. Variability is checked on all of these including the longer fermi duration period. A spectralmodel will be fitted for all of these periods. It’s a mathematical formula to the shape of the source’sflux spectrum over energy. By doing this, the electron energy distribution can be understood. SpectralMaps will then give a plot of the number of contributing photons from the source, of a given period.It also shows how well the models are adjusted to other light sources in the field of view. To get thecollected data from relevant catalogs, together with Fermi data from this analysis. A Spectral EnergyDistribution is downloaded from [Sed builder. [Online]. Available: https://tools.ssdc.asi.it/SED/] provided by the Italian space agency. The modelling is done toget an idea of the physical parameters present in the AGN. Such as the physical scales and proportionsof the structure near the core. Data from the SED will be used in the modelling with the best suitedperiod for the Fermi-LAT range.

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Zangarelli, Riccardo. "Processi di scattering in astrofisica". Bachelor's thesis, Alma Mater Studiorum - Università di Bologna, 2020. http://amslaurea.unibo.it/21201/.

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L'elaborato contiene una descrizione generale dei principali processi di scattering di importanza astrofisica, a partire dal più semplice fenomeno di scattering Thomson; si prosegue con lo scattering Compton e inverse Compton, del quale si evidenzia la relazione con il sincrotrone (synchrotron self-Compton). Viene analizzata l'evoluzione di uno spettro dominato dai processi Compton e inverse Compton (Comptonizzazione), e si conclude la trattazione dei processi in sè con una breve descrizione dello scattering ad opera della polvere. Infine, vengono esposti degli esempi di applicazioni dei processi in modo da giustificare l'importanza astrofisica di questi ultimi.

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Macconi, Duccio. "Processi di scattering in astrofisica". Bachelor's thesis, Alma Mater Studiorum - Università di Bologna, 2016. http://amslaurea.unibo.it/11466/.

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L'attenzione è stata posta su tre fenomeni fondamentali di scattering: Thomson, Compton e Compton inverso. Sono state sottolineate alcune ed eventuali applicazioni astrofisiche di questi e valutate le implicazioni o generalizzazioni che da tali fenomeni possono derivare: Synchrotron Self-Compton, Comptonizzazione ed effetto Sunyaev-Zeldovich termico. Infine è stato preso un caso astrofisico come applicazione di questi fenomeni: Sagittarius A*, una fonte radio proveniente dal centro della nostra galassia, molto studiata negli anni, citando un articolo pubblicato su una rivista scientifica nel 2012.

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Cerqui, Valeria. "Processi di scattering in astrofisica". Bachelor's thesis, Alma Mater Studiorum - Università di Bologna, 2018. http://amslaurea.unibo.it/15545/.

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Lo scattering, o diffusione, è un processo di interazione tra radiazione e materia. In particolare a livello astrofisico i processi rilevanti sono interazioni con particelle libere, solitamente elettroni. Essi vengono suddivisi in: scattering Thomson, in cui lo scattering produce solamente un cambio di direzione, lasciando invariata l'energia del fotone incidente; scattering Compton, dove il fotone incidente perde energia, trasferendola all'elettrone; Compton inverso, dove viceversa allo scattering Compton, è l'elettrone a trasferire energia al fotone incidente. Lo studio della variazione dello spettro energetico (SED) dei fotoni in caso di scattering multiplo (Compton e Inverse Compton) viene chiamato Comptonizzazione. Nel caso in cui la Comptonizzazione agisca sullo spettro della radiazione cosmica di fondo (CMB), si presenta l'effetto Sunyaev-Zel'dovich dove si ha uno shift dello spettro di corpo nero della CMB ad energie lievemente maggiori. Nel presente scritto si focalizzerà l'attenzione sulla profondità ottica Thomson, che si presta a varie applicazioni astrofisiche. Nello specifico verrà trattato il caso di scattering Thomson nell'ambiente delle symbiotic stars (SS) e come la profondità ottica vari a seconda delle fasi del sistema binario.

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De, Nichilo Elisa. "Processi di scattering in astrofisica". Bachelor's thesis, Alma Mater Studiorum - Università di Bologna, 2021. http://amslaurea.unibo.it/23916/.

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Con il termine scattering si definisce un processo fisico che descrive l’interazione di una particella con la radiazione elettromagnetica; in base all’energia coinvolta nel processo, si possono identificare diverse tipologie di scattering che vengono descritte nel primo capitolo di questo elaborato. Un caso estremamente rilevante è lo scattering Thomson, dove un elettrone in quiete subisce un urto elastico con un fotone di bassa energia che viene diffuso con una frequenza pari a quella iniziale. Per energie elevate l'effetto dominante è lo scattering Compton. In questo meccanismo un fotone, effettuando un urto elastico con un elettrone, trasferisce ad esso parte della sua energia e diminuisce la sua frequenza. Al contrario, se è l'elettrone a trasferire parte della sua energia al fotone, si parla di Inverse Compton. Quando i fotoni appartenenti alla radiazione di sincrotrone effettuano scattering con elettroni relativistici, si ha Synchrotron Self-Compton. I processi di scattering Compton e Compton Inverso si possono riassumere in un fenomeno più generale chiamato Comptonizzazione, che concerne le modifiche sullo spettro di radiazione avvenute in seguito all'interazione Compton tra fotoni ed elettroni. Un caso specifico di Comptonizzazione è l’effetto Sunyaev-Zeldovich che riguarda i fotoni della Radiazione Cosmica di Fondo. Nel secondo capitolo si esaminano alcuni esempi in cui lo scattering riveste un ruolo importante nella Fisica dell’accrescimento: la Luminosità di Eddington, per cui è importante introdurre il concetto di sezione d’urto di Thomson, e l'emissione in banda X della radiazione elettromagnetica in seguito a Comptonizzazione, che ha sede nelle regioni coronali dei buchi neri.

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Andersson, Tom. "Inverse Compton gamma-rays from Markarian 421 : A study of GeV and TeV emission from Mrk 421 based on Fermi-LAT and H.E.S.S. data". Thesis, Linnéuniversitetet, Institutionen för fysik och elektroteknik (IFE), 2016. http://urn.kb.se/resolve?urn=urn:nbn:se:lnu:diva-57861.

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This thesis summarizes a senior project on the Active Galactic Nucleus (AGN) Markarian 421 (Mrk 421). Observations of Gev and TeV flux with Fermi Large Area Telescope (LAT) and High Energy Stereoscopic System (H.E.S.S.) were compared with previous reports and publications of flux analyses of the gamma-ray emission from Mrk 421. Power laws with exponential cutoffs made consistent fits to most SEDs in the GeV and TeV bands.

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Fransson, Emma. "High energy gamma ray emission and multi-wavelength view of the AGN PKS 0537-441". Thesis, Linnéuniversitetet, Institutionen för fysik och elektroteknik (IFE), 2017. http://urn.kb.se/resolve?urn=urn:nbn:se:lnu:diva-66894.

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This thesis describes the analysis of Very High Energy (VHE) emission from the Active Galactic Nucleus PKS 0537-441. It also aims to put the results in a wider context by implementing previous work done on this source. The data chosen for the analysis is provided by the Fermi-LAT satellite and covers the energy range between 300 MeV and 300 GeV. Initially a lightcurve of the received ﬂux from the source was generated, containing data from August 2008 to April 2017, with a mean ﬂux of 4∗10−8 photons per second per squared centimeter. The lightcurve contained sections of diﬀerent ﬂux intensities giving periods of special interest, such as a ﬂaring period at August 2008 to August 2011, an enormous ﬂare at April 2010 and a less active period between April 2013 - January 2016 that could be identiﬁed for further investigations. The diﬀerences in observed ﬂux over time was tested and PKS 0537-441 was found to be a signiﬁcantly variable source. Spectral Energy Distribution (SED) analysis was performed over both the entire period as well as over the selected subperiods and ﬁtted against models using the tools provided by the Fermi Science Support Center (FSSC). The models used in the ﬁtting was PowerLaw2, LogParabola and PLSuperExpCutoﬀ and the best ﬁt for the data was obtained from the PLSuperExpCutoﬀ, except for the less intense period where the LogParabola gave the best ﬁt. The result from the SED analysis was integrated with results from previous work done on the source, ranging over multiple wavelengths in order to get a SED which spanned over the entire electromagnetic spectrum. Finally, modeling of this multi wavelength SED was performed in order to obtain parameters for the physical processes involved in the creation of the radiation received from PKS 0537-441.

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Części książek na temat "Synchrotron Self Compton (SSC)"

Ghisellini, Gabriele. "Synchrotron Self-Compton". W Radiative Processes in High Energy Astrophysics, 89–93. Heidelberg: Springer International Publishing, 2013. http://dx.doi.org/10.1007/978-3-319-00612-3_6.

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Derishev, E. V., V. V. Kocharovsky, Vl V. Kocharovsky i P. Mészáros. "GRB Synchrotron-Self-Compton Emission Generated by Self-Consistent Electron Distribution". W Gamma-Ray Bursts in the Afterglow Era, 327–29. Berlin, Heidelberg: Springer Berlin Heidelberg, 2003. http://dx.doi.org/10.1007/10853853_87.

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Streszczenia konferencji na temat "Synchrotron Self Compton (SSC)"

Bloom, Steven D., i Alan P. Marscher. "Examining the synchrotron self-Compton model for blazars". W COMPTON GAMMA-RAY OBSERVATORY. AIP, 1993. http://dx.doi.org/10.1063/1.44288.

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Anjum, Muhammad S., i Joni Tammi. "Nonlinear synchrotron self-compton modelling of blazars". W 2015 Fourth International Conference on Aerospace Science and Engineering (ICASE). IEEE, 2015. http://dx.doi.org/10.1109/icase.2015.7489524.

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Resmi, Lekshmi, Bing Zhang, J. E. McEnery, J. L. Racusin i N. Gehrels. "Gamma Ray Burst Prompt Emission Variability in Synchrotron and Synchrotron Self-Compton Lightcurves". W GAMMA RAY BURSTS 2010. AIP, 2011. http://dx.doi.org/10.1063/1.3621746.

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Finke, Justin D., Charles D. Dermer, Markus Böttcher, M. Galassi, David Palmer i Ed Fenimore. "Nonthermal Synchrotron and Synchrotron Self-Compton Emission from GRBs: Predictions for Swift and GLAST". W GAMMA-RAY BURSTS 2007: Proceedings of the Santa Fe Conference. AIP, 2008. http://dx.doi.org/10.1063/1.2943490.

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Joshi, Jagdish C., Vikas Chand i Soebur Razzaque. "Synchrotron and synchrotron self-Compton emission components in GRBs detected at very high energies". W Proceedings of the MG16 Meeting on General Relativity. WORLD SCIENTIFIC, 2023. http://dx.doi.org/10.1142/9789811269776_0243.

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Kocharovsky, Vl V. "Effects of self-Compton cooling on the synchrotron spectrum of GRBs". W RELATIVISTIC ASTROPHYSICS: 20th Texas Symposium. AIP, 2001. http://dx.doi.org/10.1063/1.1419625.

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Derishev, E. V. "Self-consistent cooling and synchrotron-self-Compton emission of relativistic electrons in gamma-ray bursts". W Cosmology and particle physics. AIP, 2001. http://dx.doi.org/10.1063/1.1363563.

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Derishev, E. V. "The Self-Consistent keV to TeV Spectra of Gamma-Ray Bursts Produced by the Synchrotron-Self-Compton Emission in Relativistic Shocks". W GAMMA-RAY BURST AND AFTERGLOW ASTRONOMY 2001: A Workshop Celebrating the First Year of the HETE Mission. AIP, 2003. http://dx.doi.org/10.1063/1.1579362.

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Coriat, M., S. Corbel, M. M. Buxton, C. D. Baylin, Jéro^me Rodriguez i Phillippe Ferrando. "Broadband Correlations Provide Evidence for Synchrotron Self-Compton X-rays from the Black Hole Binary GX 339–4". W SIMBOL-X: FOCUSING ON THE HARD X-RAY UNIVERSE: Proceedings of the 2nd International Simbol-X Symposium. AIP, 2009. http://dx.doi.org/10.1063/1.3149414.

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SINITSYNA, V. G., A. Y. ALAVERDIAN, A. S. BOLDYREV, S. S. BORISOV, R. M. MIRSAFATIKHOV i V. Y. SINITSYNA. "VHE SPECTRAL ENERGY DISTRIBUTION OF CRAB NEBULA COMPARED WITH THE PREDICTION OF A SYNCHROTRON SELF-COMPTON EMISSION MODEL". W Proceedings of the 12th ICATPP Conference. WORLD SCIENTIFIC, 2011. http://dx.doi.org/10.1142/9789814329033_0001.

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