Exomoons are predicted to produce transit timing variations (TTVs) upon their host planet. Unfortunately, so are many other astrophysical phenomena - most notably other planets in the system. In this work, an argument of reductio ad absurdum is invoked, by deriving the transit timing effects that are impossible for a single exomoon to produce. Our work derives three key analytic tests. First, one may exploit the fact that a TTV signal from an exomoon should be accompanied by transit duration variations (TDVs), and that one can derive a TDV floor as a minimum expected level of variability. Cases for which the TDV upper limit is below this floor can thus be killed as exomoon candidates. Second, formulae are provided for estimating whether moons are expected to be "killable" when no TDVs presently exist, thus enabling the community to estimate the value of deriving TDVs beforehand. Third, a TTV ceiling is derived, above which exomoons should never be able to produce TTV amplitudes. These tools are applied to a catalog of TTVs and TDVs for two and half thousand Kepler Objects of Interest, revealing over two hundred cases that cannot be due to a moon - remarkably then a large fraction of the known TTV amplitudes are consistent with being caused by a moon. These tests are also applied to the exomoon candidate Kepler-1625b i, which comfortably passes the criteria. These simple analytic results should provide a means of rapidly rejecting putative exomoons and streamlining the search for satellites.
{"title":"Impossible moons - transit timing effects that cannot be due to exomoon","authors":"D. Kipping, A. Teachey","doi":"10.2298/saj2001025k","DOIUrl":"https://doi.org/10.2298/saj2001025k","url":null,"abstract":"Exomoons are predicted to produce transit timing variations (TTVs) upon\u0000 their host planet. Unfortunately, so are many other astrophysical phenomena\u0000 - most notably other planets in the system. In this work, an argument of\u0000 reductio ad absurdum is invoked, by deriving the transit timing effects that\u0000 are impossible for a single exomoon to produce. Our work derives three key\u0000 analytic tests. First, one may exploit the fact that a TTV signal from an\u0000 exomoon should be accompanied by transit duration variations (TDVs), and\u0000 that one can derive a TDV floor as a minimum expected level of variability.\u0000 Cases for which the TDV upper limit is below this floor can thus be killed as\u0000 exomoon candidates. Second, formulae are provided for estimating whether\u0000 moons are expected to be \"killable\" when no TDVs presently exist, thus\u0000 enabling the community to estimate the value of deriving TDVs beforehand.\u0000 Third, a TTV ceiling is derived, above which exomoons should never be able\u0000 to produce TTV amplitudes. These tools are applied to a catalog of TTVs and\u0000 TDVs for two and half thousand Kepler Objects of Interest, revealing over\u0000 two hundred cases that cannot be due to a moon - remarkably then a large\u0000 fraction of the known TTV amplitudes are consistent with being caused by a\u0000 moon. These tests are also applied to the exomoon candidate Kepler-1625b i,\u0000 which comfortably passes the criteria. These simple analytic results should\u0000 provide a means of rapidly rejecting putative exomoons and streamlining the\u0000 search for satellites.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2020-04-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"44044774","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Photometric observations in g' and i' bands of the newly-discovered W UMa stars WISEJ004327.7+722407 and WISEJ234557.8+510456 are presented. The two targets are with shallow-contact configurations and their components are of G{K spectral type. We found that WISEJ004327.7+722407 is of A subtype while WISEJ234557.8+510456 is of W subtype. The different light levels at the quadratures were reproduced by cool spots on the bigger components. The procedure for calculation of the global parameters of eclipsing binaries by light curve solutions and GAIA distances was refined for stars with deep eclipses. The obtained global parameters reveal that at least one of the components of WISEJ004327.7+722407 and WISEJ234557.8+510456 is oversized, overluminous and too hot compared with an MS star with the same mass.
{"title":"Global parameters of the newly-discovered W UMa stars WISEJ004327.7+722407 and WISEJ234557.8+510456","authors":"D. Kjurkchieva, S. Ibryamov","doi":"10.2298/saj2000019k","DOIUrl":"https://doi.org/10.2298/saj2000019k","url":null,"abstract":"Photometric observations in g' and i' bands of the newly-discovered W UMa stars WISEJ004327.7+722407 and WISEJ234557.8+510456 are presented. The two targets are with shallow-contact configurations and their components are of G{K spectral type. We found that WISEJ004327.7+722407 is of A subtype while WISEJ234557.8+510456 is of W subtype. The different light levels at the quadratures were reproduced by cool spots on the bigger components. The procedure for calculation of the global parameters of eclipsing binaries by light curve solutions and GAIA distances was refined for stars with deep eclipses. The obtained global parameters reveal that at least one of the components of WISEJ004327.7+722407 and WISEJ234557.8+510456 is oversized, overluminous and too hot compared with an MS star with the same mass.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2020-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68674348","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
We present a short biography and brief review of contributions of professor Mirjana Vukicevic-Karabin to the development of astrophysics education at the University of Belgrade and to the research in physics of the Earth ionosphere and the Sun. The bibliography of her papers is given as well. We hope that the review of the two aspects of her work will elucidate her important role in the development of astrophysics in our country
{"title":"Life, educational and scientific activities of professor Mirjana Vukicevic-Karabin (1933-2020)","authors":"I. Vince, O. Atanacković","doi":"10.2298/saj2001049v","DOIUrl":"https://doi.org/10.2298/saj2001049v","url":null,"abstract":"We present a short biography and brief review of contributions of professor Mirjana Vukicevic-Karabin to the development of astrophysics education at the University of Belgrade and to the research in physics of the Earth ionosphere and the Sun. The bibliography of her papers is given as well. We hope that the review of the two aspects of her work will elucidate her important role in the development of astrophysics in our country","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2020-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68674682","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
We determined Weierstrass canonical form of cosmic time formula in the cases of four-component and some three-component universe, assuming the ?CDM model. In all other cases, we discussed analytical solutions for the cosmic time formula.
{"title":"Cosmic time for multi-component universe","authors":"D. Branković","doi":"10.2298/saj2001015b","DOIUrl":"https://doi.org/10.2298/saj2001015b","url":null,"abstract":"We determined Weierstrass canonical form of cosmic time formula in the cases of four-component and some three-component universe, assuming the ?CDM model. In all other cases, we discussed analytical solutions for the cosmic time formula.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2020-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68674456","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The evolution of massive stars in close binary systems is significantly different from single star evolution due to a series of interactions between the two stellar components. Such massive close binary systems are linked to various astrophysical phenomena, for example Wolf-Rayet stars, supernova type Ib and Ic, X-ray binaries and gamma-ray bursts. Also, the emission of gravitational waves, recently observed by the LIGO-Virgo detectors, is associated with mergers in binary systems containing compact objects, relics of massive stars - black holes and neutron stars. Evolutionary calculations of massive close binary systems were performed by various authors, but many aspects are not yet fully understood. In this paper, the main concepts of massive close binary evolution are reviewed, together with the most important parameters that can influence the final outcome of the binary system evolution, such as rotation, magnetic fields, stellar wind mass loss and mass accretion efficiency during interactions. An extensive literature overview of massive close binary models in the light of exciting observations connected with those systems is presented.
{"title":"The evolution of massive binary systems","authors":"J. Petrovic","doi":"10.2298/saj2001001p","DOIUrl":"https://doi.org/10.2298/saj2001001p","url":null,"abstract":"The evolution of massive stars in close binary systems is significantly different from single star evolution due to a series of interactions between the two stellar components. Such massive close binary systems are linked to various astrophysical phenomena, for example Wolf-Rayet stars, supernova type Ib and Ic, X-ray binaries and gamma-ray bursts. Also, the emission of gravitational waves, recently observed by the LIGO-Virgo detectors, is associated with mergers in binary systems containing compact objects, relics of massive stars - black holes and neutron stars. Evolutionary calculations of massive close binary systems were performed by various authors, but many aspects are not yet fully understood. In this paper, the main concepts of massive close binary evolution are reviewed, together with the most important parameters that can influence the final outcome of the binary system evolution, such as rotation, magnetic fields, stellar wind mass loss and mass accretion efficiency during interactions. An extensive literature overview of massive close binary models in the light of exciting observations connected with those systems is presented.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2020-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68674367","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
D. Vujičić, R. Pavlović, D. Milosevic, B. Djordjevic, S. Randjić, Dijana Stojić
This paper describes an artificial neural network for classification of asteroids into families. The data used for artificial neural network training and testing were obtained by the Hierarchical Clustering Method (HCM). We have shown that an artificial neural networks can be used as a validation method for the HCM on families with a large number of members.
{"title":"Classification of asteroid families with artificial neural networks","authors":"D. Vujičić, R. Pavlović, D. Milosevic, B. Djordjevic, S. Randjić, Dijana Stojić","doi":"10.2298/saj2001039v","DOIUrl":"https://doi.org/10.2298/saj2001039v","url":null,"abstract":"This paper describes an artificial neural network for classification of asteroids into families. The data used for artificial neural network training and testing were obtained by the Hierarchical Clustering Method (HCM). We have shown that an artificial neural networks can be used as a validation method for the HCM on families with a large number of members.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.5,"publicationDate":"2020-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68674601","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The Yarkovsky effect is an important force to consider in order to understand the long-term dynamics of asteroids. This non-gravitational force affects the orbital elements of objects revolving around a source of heat, especially their semi-major axes. Following the recently defined `limiting' value of the Yarkovsky drift speed at 7x10-5 au/Myr in Milic Zitnik (2019) (below this value of speed asteroids typically jump quickly across the mean motion resonances), we decided to investigate the relation between the asteroid family Yarkovsky V-shape and the `limiting' Yarkovsky drift speed of asteroid's semi-major axes. We have used the known scaling formula to calculate the Yarkovsky drift speed (Spoto et al. 2015) in order to determine the inner and outer `limiting' diameters (for the inner and outer V-shape borders) from the `limiting' Yarkovsky drift speed. The method was applied to 11 asteroid families of different taxonomic classes, origin type and age, located throughout the Main Belt. Here, we present the results of our calculation on relationship between asteroid families' V-shapes (crossed by strong and/or weak mean motion resonances) and the `limiting' diameters in the (a, 1=D) plane. Our main conclusion is that the `breakpoints' in changing V-shape of the very old asteroid families, crossed by relatively strong mean motion resonances on both sides very close to the parent body, are exactly the inverse of `limiting' diameters in the a versus 1=D plane. This result uncovers a novel interesting property of asteroid families' Yarkovsky V-shapes.
为了理解小行星的长期动力学，亚尔科夫斯基效应是一个需要考虑的重要因素。这种非引力影响着围绕热源旋转的物体的轨道元素，尤其是它们的半长轴。根据Milic Zitnik(2019)最近定义的Yarkovsky漂移速度的“极限”值为7x10-5 au/Myr(低于此速度的小行星通常会快速跳过平均运动共振)，我们决定研究小行星家族Yarkovsky v形与小行星半长轴的“极限”Yarkovsky漂移速度之间的关系。我们使用已知的缩放公式来计算Yarkovsky漂移速度(Spoto et al. 2015)，以便从“极限”Yarkovsky漂移速度确定内部和外部“极限”直径(用于内部和外部v形边界)。该方法应用于位于主带的11个不同分类类别、起源类型和年龄的小行星科。在这里，我们展示了我们对小行星家族的v形(由强和/或弱平均运动共振交叉)与(a, 1=D)平面上的“极限”直径之间关系的计算结果。我们的主要结论是，非常古老的小行星家族改变v形的“断点”，在非常靠近母体的两侧相对较强的平均运动共振，正好是a与1=D平面上“极限”直径的反比。这一结果揭示了小行星家族Yarkovsky v型的一个新奇有趣的特性。
{"title":"The relationship between the `limiting' Yarkovsky drift speed and asteroid families' Yarkovsky V-shape","authors":"I. Milic-Zitnik","doi":"10.2298/saj2000025m","DOIUrl":"https://doi.org/10.2298/saj2000025m","url":null,"abstract":"The Yarkovsky effect is an important force to consider in order to understand the long-term dynamics of asteroids. This non-gravitational force affects the orbital elements of objects revolving around a source of heat, especially their semi-major axes. Following the recently defined `limiting' value of the Yarkovsky drift speed at 7x10-5 au/Myr in Milic Zitnik (2019) (below this value of speed asteroids typically jump quickly across the mean motion resonances), we decided to investigate the relation between the asteroid family Yarkovsky V-shape and the `limiting' Yarkovsky drift speed of asteroid's semi-major axes. We have used the known scaling formula to calculate the Yarkovsky drift speed (Spoto et al. 2015) in order to determine the inner and outer `limiting' diameters (for the inner and outer V-shape borders) from the `limiting' Yarkovsky drift speed. The method was applied to 11 asteroid families of different taxonomic classes, origin type and age, located throughout the Main Belt. Here, we present the results of our calculation on relationship between asteroid families' V-shapes (crossed by strong and/or weak mean motion resonances) and the `limiting' diameters in the (a, 1=D) plane. Our main conclusion is that the `breakpoints' in changing V-shape of the very old asteroid families, crossed by relatively strong mean motion resonances on both sides very close to the parent body, are exactly the inverse of `limiting' diameters in the a versus 1=D plane. This result uncovers a novel interesting property of asteroid families' Yarkovsky V-shapes.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":"56 1","pages":"25-41"},"PeriodicalIF":0.5,"publicationDate":"2020-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"68674356","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
We present results from long-term optical photometric and spectroscopic observations of five pre-main sequence stars, located in the vicinity of the bright nebula NGC 7129. We obtained UBVRI photometric observations in the field centered on the star V391 Cep, north-west of the bright nebula NGC 7129. Our multicolor CCD observations spanned the period from February 1998 to November 2016. At the time of our photometric monitoring, a total of thirteen medium-resolution optical spectra of the stars were obtained. The results from our photometric study show that all stars exhibit strong variability in all optical passbands. Long-term light curves of the five stars indicate the typical classical T Tauri star variations in brightness with large amplitudes. We did not find any reliable periodicity in the brightness variations of all five stars. The results from spectral observations showed that all studied stars can be classified as classical T Tauri stars with rich emission line spectra and strong variability in profiles and intensity of emission lines.
{"title":"Photometric and spectroscopic study of five pre-main sequence stars in the vicinity of NGC 7129","authors":"E. Semkov, S. Ibryamov, S. Peneva","doi":"10.2298/SAJ1999039S","DOIUrl":"https://doi.org/10.2298/SAJ1999039S","url":null,"abstract":"We present results from long-term optical photometric and spectroscopic\u0000 observations of five pre-main sequence stars, located in the vicinity of the\u0000 bright nebula NGC 7129. We obtained UBVRI photometric observations in the\u0000 field centered on the star V391 Cep, north-west of the bright nebula NGC\u0000 7129. Our multicolor CCD observations spanned the period from February 1998\u0000 to November 2016. At the time of our photometric monitoring, a total of\u0000 thirteen medium-resolution optical spectra of the stars were obtained. The\u0000 results from our photometric study show that all stars exhibit strong\u0000 variability in all optical passbands. Long-term light curves of the five\u0000 stars indicate the typical classical T Tauri star variations in brightness\u0000 with large amplitudes. We did not find any reliable periodicity in the\u0000 brightness variations of all five stars. The results from spectral\u0000 observations showed that all studied stars can be classified as classical T\u0000 Tauri stars with rich emission line spectra and strong variability in\u0000 profiles and intensity of emission lines.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":" ","pages":""},"PeriodicalIF":0.5,"publicationDate":"2019-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"49345971","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Galaxies represent the main form of organization of matter in our universe. Therefore, they are of obvious interest for the new multidisciplinary field of astrobiology. In particular, to study habitability of galaxies represents one of the main emerging challenges of theoretical and numerical astrobiology. Its theoretical underpinnings are, however, often confused and vague. Here we present a systematic attempt to list and categorize major causal factors playing a role in emergent habitability of galaxies. Furthermore, we argue that the methodology of cosmological merger trees is particularly useful in delineating what are systematic and lawful astrobiological properties of galaxies at present epoch vs. those which are product of historical contingency and, in particular, interaction with wider extragalactic environment. Employing merger trees extracted from cosmological N-body simulations as a new and promising research method for astrobiology has been pioneered by Stanway et al. (2018). We analyse the general issue of applicability of merger trees and present preliminary results on a set of trees extracted from the Illustris Project. In a sense, this approach is directly complementary to using large-scale cosmological simulations to study habitable zones of individual galaxies with high mass/spatial resolution; taken together, they usher a new era of synergy and synthesis between cosmology and astrobiology.
{"title":"Habitability of galaxies and the application of merger trees in astrobiology","authors":"N. Stojković, B. Vukotić, M. Ćirković","doi":"10.2298/SAJ1998025S","DOIUrl":"https://doi.org/10.2298/SAJ1998025S","url":null,"abstract":"Galaxies represent the main form of organization of matter in our universe.\u0000 Therefore, they are of obvious interest for the new multidisciplinary field\u0000 of astrobiology. In particular, to study habitability of galaxies represents\u0000 one of the main emerging challenges of theoretical and numerical\u0000 astrobiology. Its theoretical underpinnings are, however, often confused and\u0000 vague. Here we present a systematic attempt to list and categorize major\u0000 causal factors playing a role in emergent habitability of galaxies.\u0000 Furthermore, we argue that the methodology of cosmological merger trees is\u0000 particularly useful in delineating what are systematic and lawful\u0000 astrobiological properties of galaxies at present epoch vs. those which are\u0000 product of historical contingency and, in particular, interaction with wider\u0000 extragalactic environment. Employing merger trees extracted from\u0000 cosmological N-body simulations as a new and promising research method for\u0000 astrobiology has been pioneered by Stanway et al. (2018). We analyse the\u0000 general issue of applicability of merger trees and present preliminary\u0000 results on a set of trees extracted from the Illustris Project. In a sense,\u0000 this approach is directly complementary to using large-scale cosmological\u0000 simulations to study habitable zones of individual galaxies with high\u0000 mass/spatial resolution; taken together, they usher a new era of synergy and\u0000 synthesis between cosmology and astrobiology.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":" ","pages":""},"PeriodicalIF":0.5,"publicationDate":"2019-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"48818089","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
In this paper, the second and the last of the series, we present a sequential algorithm to solve the stellar atmosphere problem that may serve as a paradigm for the solution of more general non-linear and non-local problems. The Iteration Factors (IF) Method is applied to achieve a solution of the radiative transfer equations, consistent with the radiative equilibrium constraint.
{"title":"The stellar atmosphere physical system II. An operative sequential algorithm to solve the stellar atmosphere problem","authors":"L. Crivellari","doi":"10.2298/SAJ190215001C","DOIUrl":"https://doi.org/10.2298/SAJ190215001C","url":null,"abstract":"In this paper, the second and the last of the series, we present a sequential algorithm to solve the stellar atmosphere problem that may serve as a paradigm for the solution of more general non-linear and non-local problems. The Iteration Factors (IF) Method is applied to achieve a solution of the radiative transfer equations, consistent with the radiative equilibrium constraint.","PeriodicalId":48878,"journal":{"name":"Serbian Astronomical Journal","volume":" ","pages":""},"PeriodicalIF":0.5,"publicationDate":"2019-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"49357540","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
京公网安备 11010802042870号
京ICP备2023020795号-1
扫码关注我们
求助内容：
应助结果提醒方式：