I review the status of the Supernova/Gamma-Ray Burst connection. Two decades of observations have established that long-duration Gamma-ray Bursts are associated with very energetic SNe-Ib/c. These SN explosions are produced by the gravitational collapse of Wolf–Rayet progenitors, with masses on the main sequence, between 30–50 $M{odot}$. Current measurements provide a GRB/SNe-Ibc ratio in the range $sim$0.02–1.5$%$, so GRBs are very rare events, even when compared with the SN frequency. There is a minority fraction of long-duration GRBs with no accompanying SN that are likely produced during the merging of neutron star or white dwarf neutron star merger.
{"title":"Supernovae and gamma-ray burst connection","authors":"M. Della Valle","doi":"10.17184/eac.7527","DOIUrl":"https://doi.org/10.17184/eac.7527","url":null,"abstract":"I review the status of the Supernova/Gamma-Ray Burst connection. Two decades of observations have established that long-duration Gamma-ray Bursts are associated with very energetic SNe-Ib/c. These SN explosions are produced by the gravitational collapse of Wolf–Rayet progenitors, with masses on the main sequence, between 30–50 $M{odot}$. Current measurements provide a GRB/SNe-Ibc ratio in the range $sim$0.02–1.5$%$, \u0000so GRBs are very rare events, even when compared with the SN frequency. There is a minority fraction of long-duration GRBs with no accompanying SN that are likely produced during the merging of neutron star or white dwarf neutron star merger.","PeriodicalId":52135,"journal":{"name":"Astronomical and Astrophysical Transactions","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2022-12-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"89701305","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"Message of the distinguished Minister of Science, Research and Technology of the Islamic Republic of Iran, His Excellency Professor Mohammad Ali Zolfigol, on the occasion of the ICRANet–Isfahan Astronomy Meeting","authors":"","doi":"10.17184/eac.7497","DOIUrl":"https://doi.org/10.17184/eac.7497","url":null,"abstract":"<jats:p />","PeriodicalId":52135,"journal":{"name":"Astronomical and Astrophysical Transactions","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2022-12-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"75692380","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
In the first observation of gravitational waves GW150914 by LIGO and Virgo [1], a binary black hole of initial black hole masses 36 units and 29 units merge into a final black hole with 62 units of mass, during which exactly 3 units of mass radiated in gravitational waves. Measuring the angular momentum carried away in gravitational waves turned out to be more challenging. This has been an open problem in classical general relativity due to ``supertranslation ambiguity" since the 1960s. Two distant observers of the same system may record different amount of "radiated angular momentum". There have been a lot of efforts to resolve the supertranslation ambiguity. One approach is to find a new definition of angular momentum that would yield the same amount of radiated angular momentum for any observer. Last year, the first such ambiguity free definition of angular momentum was discovered and it is the purpose of this note to discuss this new definition.
{"title":"Angular momentum to a distant observer","authors":"","doi":"10.17184/eac.7530","DOIUrl":"https://doi.org/10.17184/eac.7530","url":null,"abstract":"In the first observation of gravitational waves GW150914 by LIGO and Virgo [1], \u0000a binary black hole of initial black hole masses 36 units and 29 units merge into a final black hole with 62 units of mass, during which exactly 3 units of mass radiated in gravitational waves. Measuring the angular momentum carried away in gravitational waves turned out to be more challenging.\u0000This has been an open problem in classical general relativity due to ``supertranslation ambiguity\" since the 1960s. Two distant observers of the same system may record different amount of \"radiated angular momentum\". There have been a lot of efforts to resolve the supertranslation ambiguity. One approach is to find a new definition of angular momentum that would yield the same amount of radiated angular momentum for any observer. Last year, the first such ambiguity free definition of angular momentum was discovered and it is the purpose of this note to discuss this new definition.","PeriodicalId":52135,"journal":{"name":"Astronomical and Astrophysical Transactions","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2022-12-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"91109257","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
A profound difference has occurred in the analysis of GRBs initially analyzed in the domain of gamma-ray astronomy with the Compton Gamma Ray Observatory and the BATSE Detector with the extension to X-ray astronomy and optical astronomy introduced by Beppo-SAX and the KEK and VLT optical observatory, followed by the AGILE, Fermi mission, Niels Gehrels SWIFT mission as well as HEHSS and MAGIC observations. An authentic ``Copernican revolution" has occurred in the transition from the traditional model of GRBs originating in a single star progenitor (collapsar) to GRBs with a binary progenitor composed of a CO core and a companion NS. We evidence from 24 SN observations related to GRBs that all of them, once analyzed with the general relativistic corrections, can be identified with I Bc Sn with a common value of the luminosity and common time of occurrence of the peak of the optical emission. This can be understood in terms of a precursor composed of a CO core and a binary NS companion. By contrast, the GRBs differ profoundly in their energetics which can be expressed in terms of 3 different classes of BDHNe: BDHN I, BDHN II, BDHN III, also originating from precursors composed of a CO core and a binary companion. It is pointed out how the analysis of these systems has profoundly modified the concept of the BH and the associated fundamental physics necessary for their description since the publication of ``Introducing the Black Hole" by Ruffini and Wheeler in 1971. At first, it is illustrated how the most radical change has occurred in the introduction of the effective BH charge, with an electric field only function of the BH dimensionless spin and a background magnetic field $B0$. This definitely indicates the abandonment of the Kerr--Newman solution in favour of the Kerr metric, for energy extraction processes in BH physics. We then enter in the detailed description of the ``seven Seals", the seven Episodes characterizing GRB 190114c and the associated SN 2019jrj. Based on the article by Aimuratov et al., in preparation.
从康普顿伽玛射线天文台和BATSE探测器最初在伽玛射线天文学领域进行的伽玛射线暴分析，到Beppo-SAX、KEK和VLT光学天文台引入的x射线天文学和光学天文学的扩展，再到AGILE、费米任务、Niels Gehrels SWIFT任务以及HEHSS和MAGIC观测，发生了深刻的变化。一场真正的“哥白尼革命”发生在传统的伽玛暴模型的转变过程中，即从起源于单星祖先(坍缩星)的伽玛暴转变为由CO核心和伴星NS组成的双星祖先的伽玛暴。我们从与grb相关的24个SN观测中证明，一旦用广义相对论修正分析，它们都可以与具有共同光度值和共同光发射峰出现时间的I Bc SN相识别。这可以用由CO核和二元NS伴体组成的前驱体来理解。相比之下，grb的能量学差异很大，可以用3种不同类型的BDHN来表达:BDHN I, BDHN II, BDHN III，它们也起源于由CO核心和双星伴星组成的前体。文章指出，自Ruffini和Wheeler于1971年发表“介绍黑洞”以来，对这些系统的分析如何深刻地改变了黑洞的概念以及描述黑洞所必需的相关基础物理学。首先，它说明了最根本的变化是如何在引入有效黑洞电荷时发生的，电场仅是黑洞无量纲自旋和背景磁场的函数。这明确表明，在黑洞物理的能量提取过程中，克尔-纽曼解被克尔度规所取代。然后，我们输入“七个封印”的详细描述，即描述GRB 190114c和相关SN 2019jrj的七个章节。根据Aimuratov等人的文章，在编写。
{"title":"On the nature of the ultrarelativistic prompt emission phase of GRB 190114C and GRB 180720B","authors":"R. Ruffini","doi":"10.17184/eac.7523","DOIUrl":"https://doi.org/10.17184/eac.7523","url":null,"abstract":"A profound difference has occurred in the analysis of GRBs initially analyzed in the domain of gamma-ray astronomy with the Compton Gamma Ray Observatory and the BATSE Detector with the extension to X-ray astronomy and optical astronomy introduced by Beppo-SAX and the KEK and VLT optical observatory, followed by the AGILE, Fermi mission, Niels Gehrels SWIFT mission as well as HEHSS and MAGIC observations. \u0000An authentic ``Copernican revolution\" has occurred in the transition from the traditional model of GRBs originating in a single star progenitor (collapsar) to GRBs with a binary progenitor composed of a CO core and a companion NS. \u0000We evidence from 24 SN observations related to GRBs that all of them, once analyzed with the general relativistic corrections, can be identified with I Bc Sn with a common value of the luminosity and common time of occurrence of the peak of the optical emission. This can be understood in terms of a precursor composed of a CO core and a binary NS companion. By contrast, the GRBs differ profoundly in their energetics which can be expressed in terms of 3 different classes of BDHNe: BDHN I, BDHN II, BDHN III, also originating from precursors composed of a CO core and a binary companion.\u0000It is pointed out how the analysis of these systems has profoundly modified the concept of the BH and the associated fundamental physics necessary for their description since the \u0000publication of ``Introducing the Black Hole\" by Ruffini and Wheeler in 1971. At first, it is illustrated how the most radical change has occurred in the introduction of the effective BH charge, with an electric field only function of the BH dimensionless spin and a background magnetic field $B0$. This definitely indicates the abandonment of the Kerr--Newman solution in favour of the Kerr metric, for energy extraction processes in BH physics. We then enter in the detailed description of the ``seven Seals\", the seven Episodes characterizing GRB 190114c and the associated SN 2019jrj.\u0000\u0000Based on the article by Aimuratov et al., in preparation.","PeriodicalId":52135,"journal":{"name":"Astronomical and Astrophysical Transactions","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2022-12-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"81116521","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Mathematical and astronomical achievements of the Islamic world during its golden era are briefly exposed. The article is based on the invited talk delivered remotely at the ICRANET–Isfahan Astronomical Meeting, November 2–5, 2021, which, in turn, reproduces major parts of one of the chapters of my book ``Our Celestial Clockwork'', published recently (2021) by the World Scientific.
{"title":"Astronomy in the Islamic world: a European perspective","authors":"R. Kerner","doi":"10.17184/eac.7525","DOIUrl":"https://doi.org/10.17184/eac.7525","url":null,"abstract":"Mathematical and astronomical achievements of the Islamic world during its golden era are briefly exposed. \u0000The article is based on the invited talk delivered remotely at the ICRANET–Isfahan Astronomical Meeting,\u0000November 2–5, 2021, which, in turn, reproduces major parts of one of the chapters of my book ``Our Celestial\u0000Clockwork'', published recently (2021) by the World Scientific.","PeriodicalId":52135,"journal":{"name":"Astronomical and Astrophysical Transactions","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2022-12-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"83489505","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
C. Argüelles, E. A. Becerra-Vergara, V. Crespi, A. Krut, J. Rueda, R. Ruffini, R. Yunis
The transition from linear to non-linear structure formation in cosmology is here studied from the point of view of the thermodynamics of self-gravitating fermions. We start by reviewing the principle of maximum entropy production through which such a fermionic system can relax towards spherical equilibrium states able to explain the dark matter (DM) in galaxies. We then analyze the stability, lifetime and morphology of the above configurations, and show that the most general DM profile develops a compact core governed by degeneracy pressure, which is surrounded by an extended halo. For DM particles which are in the range of $mathcal{O}$(10--100) keV, we apply this theory to the case of the Milky Way, and show that the compact DM-core explains the dynamics of all the best resolved S-cluster stars orbiting SgrA *, without the need of assuming a central black hole (BH). Further consequences of this theory regarding open issues in cosmology are outlined, including the problem of formation of supermassive BHs in the early Universe.
{"title":"Dark matter fermions: from linear to non-linear structure formation","authors":"C. Argüelles, E. A. Becerra-Vergara, V. Crespi, A. Krut, J. Rueda, R. Ruffini, R. Yunis","doi":"10.17184/eac.7532","DOIUrl":"https://doi.org/10.17184/eac.7532","url":null,"abstract":"The transition from linear to non-linear structure formation in cosmology is here studied from the point of view of the thermodynamics of self-gravitating fermions. We start by reviewing the principle of maximum entropy production through which such a fermionic system can relax towards spherical equilibrium states able to explain the dark matter (DM) in galaxies. We then analyze the stability, lifetime and morphology of the above configurations, and show that the most general DM profile develops a compact core governed by degeneracy pressure, which is surrounded by an extended halo. For DM particles which are in the range of $mathcal{O}$(10--100) keV, we apply this theory to the case of the Milky Way, and show that the compact DM-core explains the dynamics of all the best resolved S-cluster stars orbiting SgrA *, without the need of assuming a central black hole (BH). Further consequences of this theory regarding open issues in cosmology are outlined, including the problem of formation of supermassive BHs in the early Universe.","PeriodicalId":52135,"journal":{"name":"Astronomical and Astrophysical Transactions","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2022-12-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"90491006","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
In the framework of Randall–Sundrum theory with extra dimension Reissner–Nordstrom black hole solutions with a tidal charge have been found. The shadow around the supermassive black hole in M87 was reconstructed in 2019 based on observations with the Event Horizon Telescope (EHT) in April 2017. In May 2022 the EHT Collaboration presented results of a shadow reconstruction for our Galactic Center. Earlier, for Reissner–Nordstrom metric we derived analytical expressions for shadow size as a function of charge and later generalized these results for a tidal charge case. We discuss opportunities to evaluate parameters of alternative theories of gravity with shadow size estimates done by the EHT Collaboration, in particular, a tidal charge could be estimated from these observations.
{"title":"Shadows around Sgr A* and M87* as a tool to test gravity theories","authors":"A. Zakharov","doi":"10.17184/eac.7531","DOIUrl":"https://doi.org/10.17184/eac.7531","url":null,"abstract":"In the framework of Randall–Sundrum theory with extra dimension Reissner–Nordstrom black hole solutions with a tidal charge have been found. The shadow around the supermassive black hole in M87 was reconstructed in 2019 based on observations with the Event Horizon Telescope (EHT) in April 2017. In May 2022 the EHT Collaboration presented results of a shadow reconstruction for our Galactic Center.\u0000Earlier, for Reissner–Nordstrom metric we derived analytical expressions for shadow size as a function of charge and later generalized these results for a tidal charge case. We discuss opportunities to evaluate parameters of alternative theories of gravity with shadow size estimates done by the EHT Collaboration, in particular, a tidal charge could be estimated from these observations.","PeriodicalId":52135,"journal":{"name":"Astronomical and Astrophysical Transactions","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2022-08-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"77413111","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"Nikolai G. Bochkarev is 75","authors":"N. Samus","doi":"10.17184/eac.6478","DOIUrl":"https://doi.org/10.17184/eac.6478","url":null,"abstract":"<jats:p />","PeriodicalId":52135,"journal":{"name":"Astronomical and Astrophysical Transactions","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2022-08-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"76864297","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
O. Antyufeyev, M. Bleiders, O. Patoka, V. Bezrukovs, I. Shmeld, V. Shulga
The method (Kraus (2007)) for correcting atmospheric opacity in the C-band was applied to the RT-16 radio telescope of the Irbene observatory. The method is based on the calculation of the noise temperature T0, which is almost independent of the environment and is determined by the characteristics of the receiver and radio telescope antenna. T0 is determined using sky dip observations. The atmospheric opacity in the zenith is calculated using T0. We have determined the time dependence of T0 over a long period of time. It is shown that the T0 error increases the error of the flux density by no more than 0.5%.
{"title":"Atmospheric opacity correction in C-band at Irbene RT-16 radio telescope","authors":"O. Antyufeyev, M. Bleiders, O. Patoka, V. Bezrukovs, I. Shmeld, V. Shulga","doi":"10.17184/eac.6473","DOIUrl":"https://doi.org/10.17184/eac.6473","url":null,"abstract":"The method (Kraus (2007)) for correcting atmospheric opacity in the C-band was applied to the RT-16 radio telescope of the Irbene observatory. The method is based on the calculation of the noise temperature T0, which is almost independent of the environment and is determined by the characteristics of the receiver and radio telescope antenna. T0 is determined using sky dip observations. The atmospheric opacity in the zenith is calculated using T0. We have determined the time dependence of T0 over a long period of time. It is shown that the T0 error increases the error of the flux density by no more than 0.5%.","PeriodicalId":52135,"journal":{"name":"Astronomical and Astrophysical Transactions","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2022-08-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"77572993","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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