Early Optical Observations of Gamma-Ray Bursts Compared with Their Gamma- and X-Ray Characteristics Using a MASTER Global Network of Robotic Telescopes from Lomonosov Moscow State University     

O. A. Ershova  V. M. Lipunov  E. S. Gorbovskoy  N. V. Tyurina  V. G. Kornilov  D. S. Zimnukhov  A. Gabovich  O. A. Gress  N. M. Budnev  V. V. Yurkov  V. V. Vladimirov  A. S. Kuznetsov  P. V. Balanutsa  R. Rebolo  M. Serra-Ricart  D. Buckley  R. Podesta  H. Levato  C. Lopez  F. Podesta  C. Francile  C. Mallamaci  S. A. Yazev  D. M. Vlasenko  A. Tlatov  V. Senik  V. Grinshpun  A. Chasovnikov  V. Topolev  A. Pozdnyakov  K. Zhirkov  D. Kuvshinov  F. Balakin 《Astronomy Reports》2020,64(2):126-158

We present the results of early observations for 130 error-boxes of gamma-ray bursts performed with the Mobile Astronomical System of TElescope-Robots (MASTER) global network of robotic telescopes from Moscow State University in fully automatic mode (2011–2017). Among them, GRB 130907A, GRB 120811C, GRB 110801A, GRB 120404A, GRB 140129B, GRB140311B, and GRB 160227A are considered in details. Among these 130 gamma-ray bursts, in the first 60 s after the trigger with the Swift, Fermi, INTEGRAL, MAXI, Lomonosov, and Konus-Wind orbital observatories, the MASTER was pointed on 51 gamma-ray bursts, being the leader in terms of the first pointing. Full observation automation and MASTER own real-time image processing software allowed us to obtain unique data on early optical emission that accompanied 44 gamma-ray bursts (GRB 110801A, GRB120106A, GRB 120404A, GRB 120811C, GRB 120907A, GRB 121011A, GRB 130122A, GRB 130907A, GRB 131030A, GRB 131125A, GRB 140103A, GRB 140108A, GRB 140129B, GRB 140206A, GRB 140304A, GRB 140311B, GRB 140512A, GRB 140629A, GRB 140801A, GRB140907A, GRB 140930B, GRB141028A, GRB 141225A, GRB 150210A, GRB 150211A, GRB 150301B, GRB 150323C, GRB 150404A/Fermi trigger 449861706, GRB 150403A, GRB 150413A, GRB 150518A, GRB 150627A, GRB 151021A, GRB 151215A, GRB 160104A, GRB 160117B, GRB 160131A, GRB 160227A, GRB 160425A, GRB 160611A, GRB 160625B, GRB 160804A, GRB 160910A, GRB 161017A, GRB 161117A, GRB 161119A). We obtain light curves for 13 gamma-ray bursts among the above listed ones and compare the data in the optical (MASTER), X-ray (Swift-XRT), and hard X-ray (Swift-BAT) ranges.  相似文献   

Search for sulfates on the surface of Ceres          下载免费PDF全文

C. Bu  G. Rodriguez Lopez  C. A. Dukes  O. Ruesch  L. A. McFadden  J.‐Y. Li 《Meteoritics & planetary science》2018,53(9):1946-1960

The formation of hydrated salts is an expected consequence of aqueous alteration of Main Belt objects, particularly for large, volatile‐rich protoplanets like Ceres. Sulfates, present on water‐bearing planetary bodies (e.g., Earth, Mars, and carbonaceous chondrite parent bodies) across the inner solar system, may contribute to Ceres’ UV and IR spectral signature along with phyllosilicates and carbonates. We investigate the presence and stability of hydrated sulfates under Ceres’ cryogenic, low‐pressure environment and the consequent spectral effects, using UV–Vis–IR reflectance spectroscopy. H₂O loss begins instantaneously with vacuum exposure, measured by the attenuation of spectral water absorption bands, and a phase transition from crystalline to amorphous is observed for MgSO₄·6H₂O by X‐ray powder diffraction. Long‐term (>40 h), continuous exposure of MgSO₄·nH₂O (n = 0, 6, 7) to low pressure (10^?3–10^?6 Torr) causes material decomposition and strong UV absorption below 0.5 μm. Our measurements suggest that MgSO₄·6H₂O grains (45–83 μm) dehydrate to 2% of the original 1.9 μm water band area over ~0.3 Ma at 200 K on Ceres and after ~42 Ma for 147 K. These rates, inferred from an Avrami dehydration model, preclude MgSO₄·6H₂O as a component of Ceres’ surface, although anhydrous and minimally hydrated sulfates may be present. A comparison between Ceres emissivity spectra and laboratory reflectance measurements over the infrared range (5–17 μm) suggests sulfates cannot be excluded from Ceres’ mineralogy.  相似文献   

Effects of pre-orogenic tectonic structures on the Cenozoic evolution of Andean deformed belts: Evidence from the Salar de Punta Negra Basin in the Central Andes of Northern Chile     

Fernando Martínez  Cristopher López  Mauricio Parra 《Basin Research》2020,32(6):1441-1462

We integrated new field observations, two-dimensional (2-D) seismic profiles and new and previously reported chronological data to understand the effects of pre-orogenic structures on the tectonic evolution of the Salar de Punta Negra in the Central Andes. For first time a series of restored geological cross-sections are presented, thus showing the pre-orogenic tectonic architecture of the region and new ideas about the tectonic evolution of the inner forearc of the Central Andes. Our results show a series of east-dipping normal faults as the main pre-orogenic structures in the region, which resulted from lithospheric stretching of the western continental margin during the Paleozoic to Mesozoic (Triassic–Jurassic). These were later incorporated into the Andean orogen by tectonic inversion, forming west-verging inversion anticlines. The beginning of the tectonic inversion is constrained by the first on-lap of the Upper Cretaceous-Palaeocene syn-kinematic deposits on the top of the Mesozoic syn-rift successions, highlighting that inversion occurred during this period. These syn-kinematic deposits display zircons with older age peaks between ca. 200 and 300 Ma, thus indicating that some Carboniferous to Triassic sources of sediments were eroded during the uplift of the orogen. Other basement reverse faults affect the footwalls of normal inverted faults and the shoulders of ancient half-graben structures. These truncate and decapitate previous inverted faults and completely cut the infill of the basin, leading to exhumation of the pre-rift basement rocks. We propose that the propagation of these structures was favoured by the modified thermal-tectonic state of the lithosphere from the eastward migration of the volcanic arc, and not by the previous pre-orogenic structures. The structural and stratigraphic relationships recognized both in the field and 2-D seismic profiles indicate that many reverse faults originated after the initial tectonic inversion and continued to be active from the Eocene until the Pleistocene period.  相似文献