標題: Titlebook: Gamma-Ray Bursts in the Afterglow Era; Proceedings of the I Enrico Costa,Filippo Frontera,Jens Hjorth Conference proceedings 2001 Springer- [打印本頁] 作者: 難免 時間: 2025-3-21 20:08
書目名稱Gamma-Ray Bursts in the Afterglow Era影響因子(影響力)
書目名稱Gamma-Ray Bursts in the Afterglow Era影響因子(影響力)學科排名
書目名稱Gamma-Ray Bursts in the Afterglow Era網絡公開度
書目名稱Gamma-Ray Bursts in the Afterglow Era網絡公開度學科排名
書目名稱Gamma-Ray Bursts in the Afterglow Era被引頻次
書目名稱Gamma-Ray Bursts in the Afterglow Era被引頻次學科排名
書目名稱Gamma-Ray Bursts in the Afterglow Era年度引用
書目名稱Gamma-Ray Bursts in the Afterglow Era年度引用學科排名
書目名稱Gamma-Ray Bursts in the Afterglow Era讀者反饋
書目名稱Gamma-Ray Bursts in the Afterglow Era讀者反饋學科排名
作者: Gingivitis 時間: 2025-3-21 23:05 作者: Adherent 時間: 2025-3-22 02:21 作者: 低三下四之人 時間: 2025-3-22 05:20 作者: mucous-membrane 時間: 2025-3-22 10:42
On the Spectra of the Gamma-Ray Bursts,Abstract. The soft tails of gamma-ray bursts spectra obtained by different instruments are discussed. It is known that some of them have excesses from the exact power law dependence. It is conjectured that this soft-excess may estimate the redshift of a long gamma-ray burst.作者: jettison 時間: 2025-3-22 15:37
Non-isotropic Angular Distribution for Very Short-Time Gamma-Ray Bursts?,We analyse the gamma-ray bursts (GRBs) . from the BATSE Catalogue. The study of the angular location of these GRBs shows .: . 1. The angular distribution is very different from the long-duration GRBs, . 2. ., consistent with a quasi-Euclidean distribution of sources. ..作者: jettison 時間: 2025-3-22 17:54
Enrico Costa,Filippo Frontera,Jens HjorthThe study of GRBs is presently a fairly hot topic in astrophysics作者: transplantation 時間: 2025-3-22 23:49
978-3-642-07668-8Springer-Verlag Berlin Heidelberg 2001作者: 劇毒 時間: 2025-3-23 04:13
Gamma-Ray Bursts in the Afterglow Era978-3-540-45505-9Series ISSN 1431-2433 Series E-ISSN 1611-6143 作者: Condyle 時間: 2025-3-23 05:45
https://doi.org/10.1007/b82840BeppoSAX; Cosmology; Gamma-Ray Bursts; Spectra of GRB; astronomy; cosmology; galaxy; gamma-ray burst; instru作者: Herbivorous 時間: 2025-3-23 14:10
Besonderheiten der bodennahen Turbulenz,poSAX data. This model gives a satisfactory description of the majority of the data. Nevertheless, . 30% need of accounting for substantial radiative cooling of the emitting electrons during the event.作者: Catheter 時間: 2025-3-23 20:13
https://doi.org/10.1007/978-3-662-53950-7 gamma-ray bursts collected at BATSE Catalog. The tests use the counts-in-cells method, an analysis of spherical harmonics, a test based on the two-point correlation function and a method based on multiscale methods. The tests suggest that the intermediate subclass of gamma-ray bursts are distributed anisotropically.作者: MEN 時間: 2025-3-23 22:54 作者: 眨眼 時間: 2025-3-24 04:01 作者: NEG 時間: 2025-3-24 06:34
https://doi.org/10.1007/978-3-540-88382-1ime are estimated for 49 long APEX bursts detected with time resolution of 0.125 sec and 16 short event detected by time-to-spill mode with time resolution of fraction of ms. The APEX data is shown to confirm the bi-modaldistribution of emission time values found for BATSE bursts.作者: 細微的差異 時間: 2025-3-24 12:21 作者: 小步舞 時間: 2025-3-24 15:07
Testing the Optically Thin Synchrotron Shock Model for Gamma-Ray Bursts Spectra from 2 to 700 keV wpoSAX data. This model gives a satisfactory description of the majority of the data. Nevertheless, . 30% need of accounting for substantial radiative cooling of the emitting electrons during the event.作者: diskitis 時間: 2025-3-24 23:04 作者: LINE 時間: 2025-3-25 01:48
Gamma-Ray Burst Follow Up Observations with BOOTES in 1998-2000,GRBs). Error box size depending, it uses wide field cameras attached to small robotic telescopes or the telescopes themselves. To date we have acquired photometry for about 30 events with the Ultra Wide (UWFC) and the Narrow Field Cameras (NFC) and about 50 events with the Wide Field Camera (WFC).作者: PLIC 時間: 2025-3-25 04:41
Tools for Gamma-Ray Burst Data Mining,al clusterings necessarily indicate separate source populations. Subclass identification can aid our understanding of systematic observationaland instrumentalbiases. We demonstrate several computational pattern-finding tools, and show how these can be applied to the problems of GRB classification and subclass interpretation.作者: Omnipotent 時間: 2025-3-25 07:42
Estimation of Emission Time Parameter for APEX Experiment,ime are estimated for 49 long APEX bursts detected with time resolution of 0.125 sec and 16 short event detected by time-to-spill mode with time resolution of fraction of ms. The APEX data is shown to confirm the bi-modaldistribution of emission time values found for BATSE bursts.作者: Irritate 時間: 2025-3-25 12:03
Angewandte Mathematik: Body and Souler the past severaly ears. The emphasis is on a) the more surprising or unusualresul ts which have not been discussed in the BATSE review talk at this meeting, and b) the energy range above about 25 keV.作者: 手工藝品 時間: 2025-3-25 16:20
Angewandte Mathematik: Body and Souls itself as a strong correlation between instantaneous energy flux . and peak energy ... In the (.,..) plane, the correlation produces distinct tracks in the form of branches and loops representing the different parts of a burst time history. Despite the variety of features seen in different events,作者: Kidnap 時間: 2025-3-25 22:58 作者: mucous-membrane 時間: 2025-3-26 02:03
Grundlegende Matrizenoperationen, but remaining undetected in the Gamma Ray Bursts Monitor on BeppoSAX. They have properties very similar to the x-ray counterparts of GRBs and account for some of the Fast X-ray Transient events seen in almost every x-ray satellite. We review their X-ray properties and show that x-ray flashes are in作者: Solace 時間: 2025-3-26 06:06 作者: 悄悄移動 時間: 2025-3-26 10:32
https://doi.org/10.1007/978-3-662-05743-8and the ProportionalCoun ter Array (PCA) instruments have detected 30 GRBs. In 16 cases, an early celestial position was released to the community, sometimes in conjunction with IPN results. The subsequent optical and radio searches led to the detection of 5 x-ray afterglows, to at least 6 optical o作者: 預兆好 時間: 2025-3-26 16:02
Besonderheiten der bodennahen Turbulenz,poSAX data. This model gives a satisfactory description of the majority of the data. Nevertheless, . 30% need of accounting for substantial radiative cooling of the emitting electrons during the event.作者: Proclaim 時間: 2025-3-26 20:19
K. Friehs,B. Hitzmann,T. Scheperell as the number of distinct pulse structures per burst. Performing the cross-correlation between two energy bands, we measure an average lag .-40 x shorter than for long bursts, and a lag distribution close to symmetric about zero - unlike long bursts. Using a “Bayesian Block” method to identify s作者: 錯誤 時間: 2025-3-26 22:32
Soziale Wohlfahrt und Sozialwahltheorie,is operating since April, 2000. When a true celestial burst is recognized, this S/W yields some relevant data, like peak counts, total counts, duration. In the near future, the possible incoming direction will be included as well. This info is promptly and automatically distributed, in a fixed forma作者: 序曲 時間: 2025-3-27 04:41 作者: babble 時間: 2025-3-27 07:43
Auseinandersetzung mit dem Produkto select among the different proposed models and possibly to identify different classes with different origins. We have tried to study the gamma light-curve behaviour in relation to other physicalparameters of the event as duration, peak counting rate, energy spectra hardness, et etc. There are hint作者: obscurity 時間: 2025-3-27 10:58
Ausgew?hlte Funktionalit?ten von ILOG ScriptGRBs). Error box size depending, it uses wide field cameras attached to small robotic telescopes or the telescopes themselves. To date we have acquired photometry for about 30 events with the Ultra Wide (UWFC) and the Narrow Field Cameras (NFC) and about 50 events with the Wide Field Camera (WFC).作者: 規(guī)章 時間: 2025-3-27 15:26
https://doi.org/10.1007/978-3-531-18886-7al clusterings necessarily indicate separate source populations. Subclass identification can aid our understanding of systematic observationaland instrumentalbiases. We demonstrate several computational pattern-finding tools, and show how these can be applied to the problems of GRB classification an作者: parasite 時間: 2025-3-27 18:01 作者: decipher 時間: 2025-3-28 01:37
Anna-Lena Majkovic,Christoph Negrihis reflects a correlation between the total emitted energies and the intrinsic durations. For the short (long) bursts the total emitted energies are roughly proportional to the first (second) power of the intrinsic duration. This difference in the energy-duration relationship is statistically signi作者: 神經 時間: 2025-3-28 03:23 作者: savage 時間: 2025-3-28 09:27 作者: ANTI 時間: 2025-3-28 10:47
Some Recent, Interesting Observations of Gamma-Ray Bursts,er the past severaly ears. The emphasis is on a) the more surprising or unusualresul ts which have not been discussed in the BATSE review talk at this meeting, and b) the energy range above about 25 keV.作者: Kidney-Failure 時間: 2025-3-28 16:22 作者: fabricate 時間: 2025-3-28 19:07 作者: 脫落 時間: 2025-3-29 01:20 作者: 價值在貶值 時間: 2025-3-29 07:06 作者: Left-Atrium 時間: 2025-3-29 08:48 作者: 我不重要 時間: 2025-3-29 15:09
Testing the Optically Thin Synchrotron Shock Model for Gamma-Ray Bursts Spectra from 2 to 700 keV wpoSAX data. This model gives a satisfactory description of the majority of the data. Nevertheless, . 30% need of accounting for substantial radiative cooling of the emitting electrons during the event.作者: tympanometry 時間: 2025-3-29 16:33
Short Gamma-Ray Bursts Are Different,ell as the number of distinct pulse structures per burst. Performing the cross-correlation between two energy bands, we measure an average lag .-40 x shorter than for long bursts, and a lag distribution close to symmetric about zero - unlike long bursts. Using a “Bayesian Block” method to identify s作者: Bumble 時間: 2025-3-29 21:38
New Possibilities Offered by BeppoSAX: Automatic GRB Alerts Using GRBM,is operating since April, 2000. When a true celestial burst is recognized, this S/W yields some relevant data, like peak counts, total counts, duration. In the near future, the possible incoming direction will be included as well. This info is promptly and automatically distributed, in a fixed forma作者: moribund 時間: 2025-3-30 00:02
Probing the Isotropy in the Sky Distribution of the Gamma-Ray Bursts, gamma-ray bursts collected at BATSE Catalog. The tests use the counts-in-cells method, an analysis of spherical harmonics, a test based on the two-point correlation function and a method based on multiscale methods. The tests suggest that the intermediate subclass of gamma-ray bursts are distribute作者: 仔細檢查 時間: 2025-3-30 04:20 作者: 一再困擾 時間: 2025-3-30 12:00 作者: aerial 時間: 2025-3-30 12:27 作者: 散步 時間: 2025-3-30 19:30 作者: 能量守恒 時間: 2025-3-30 22:12 作者: ATOPY 時間: 2025-3-31 01:20 作者: Deject 時間: 2025-3-31 05:36 作者: Filibuster 時間: 2025-3-31 11:19
Grundlegende Matrizenoperationen, fact very soft, x-ray rich, untriggered gamma ray bursts, in which the peak energy in 2-10 keV x-rays could be up to a factor of 100 larger than the peak energy in the 50-300 keV gamma ray range. The frequency is . yr..作者: Suggestions 時間: 2025-3-31 14:57
Peter Lugner,Werner Mack,Manfred Pl?chl detected in common with .SAX. Temporaland spectralc haracteristics, such as peak flux, fluence, duration, and spectrum are compared to the full population of triggered BATSE GRBs. We find that FXTs have softer spectra than most triggered bursts, but that they are consistent with the extrapolated hardness expected for low-intensity GRBs.作者: 煩憂 時間: 2025-3-31 18:26
K. Friehs,B. Hitzmann,T. Scheperignificantly distinct pulse peaks, we find an order of magnitude fewer pulses than found in studies of long bursts. The disparity in lag magnitude is discontinuous across the .-s valley between long and short bursts. Thus, short bursts do not appear to be representable as a continuation of long bursts’ temporalc haracteristics.作者: 仔細閱讀 時間: 2025-3-31 22:38 作者: OPINE 時間: 2025-4-1 02:49
X-Ray Flashes and X-Ray Rich Gamma Ray Bursts, fact very soft, x-ray rich, untriggered gamma ray bursts, in which the peak energy in 2-10 keV x-rays could be up to a factor of 100 larger than the peak energy in the 50-300 keV gamma ray range. The frequency is . yr..作者: 抱怨 時間: 2025-4-1 09:55
BATSE Observations of Fast X-Ray Transients Detected by BeppoSAX-WFC, detected in common with .SAX. Temporaland spectralc haracteristics, such as peak flux, fluence, duration, and spectrum are compared to the full population of triggered BATSE GRBs. We find that FXTs have softer spectra than most triggered bursts, but that they are consistent with the extrapolated hardness expected for low-intensity GRBs.作者: 同位素 時間: 2025-4-1 11:16
Short Gamma-Ray Bursts Are Different,ignificantly distinct pulse peaks, we find an order of magnitude fewer pulses than found in studies of long bursts. The disparity in lag magnitude is discontinuous across the .-s valley between long and short bursts. Thus, short bursts do not appear to be representable as a continuation of long bursts’ temporalc haracteristics.作者: deviate 時間: 2025-4-1 15:22 作者: 剝皮 時間: 2025-4-1 20:22 作者: 門閂 時間: 2025-4-1 22:59 作者: 巨大沒有 時間: 2025-4-2 04:52
Angewandte Mathematik: Body and Soul in the form of branches and loops representing the different parts of a burst time history. Despite the variety of features seen in different events, the main characteristics of the spectralev olution produce a quite consistent pattern.
