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The hardness ratio evolution during this observation indicated significant absorption of soft X-rays in some segments of the observation. For better understanding of the reason behind this, we performed time-resolved spectroscopy in the 2.5–10.5 keV energy band which revealed significant variations in the spectral parameters, especially the hydrogen column density and iron line equivalent width with flux. 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K., Pawar D. D. 2017, J. Astrophys. Astr., 38, 2\nAktas C., Aygun S. 2017, Chinese J. Phys., 55, 71\nBhoyar S. R., Chirde V. R., Shekh S. H. 2017, Astrophys., 60, 277\nBhoyar S., Chirde V., Shekh S. 2015, Int. J. Adv. Res., 3, 492\nBhoyar S., Chirde V., Shekh S. 2016, Prespacetime J. 7, 456\nCapozziello S., Martin-Moruno P., Rubano C. 2008, Phys. Lett. B, 664, 12\nChaubey R., Shukla A. 2013, Astrophys Space Sci., 343, 415\nChirde V., Shekh S. 2014, Bulg. J. Phys., 41, 258\nChirde V., Shekh S. 2015a, African Rev. Phys., 10, 0020\nChirde V., Shekh S. 2015b, African Rev. Phys., 10, 0057\nChirde V., Shekh S. 2015c, Astrofisica, 58, 121\nChirde V. R., Shekh S. H. 2016, J. Astrophys. Astr., 37, 15\nDrake J. J., Marshall H. L., Dreizler S. et al. 2002, Astrophys. J., 572, 996\nEinstein A. 1928, Phys. Math. Kl, 217, 401; 1930, Math. Ann. 102, 685\nFerraro R., Fiorini F. 2007, Phys. Rev. D, 75, 084031\nHarko T., Lobo F., Nojiri S., Odintsov S. 2011, Phys. Rev. D, 84, 024020\nJamil M., Momeni D., Myrzakulov R. 2012, Eur. Phys. J. C., 72, 2122\nKatore S., Chopde B., Shekh S. 2012, Int. J. Basic App. Res. (Special Issue), 283\nKatore S. D. 2012, Int. J. Theor. Phys., 51, 83\nMiranda V., Joras S., Waga I., Quartin M. 2009, Phys. Rev. Lett., 102, 221101\nNojiri S., Odintsov S. 2008, arXiv: 0807.0685 266\nPerez-Garcia M. A., Silk J., Stone J. R. 2010, Phys. Rev. Lett., 105, 141101\nRiess A. et al. 1998, Astron. J., 116, 1009\nPerlmutter S. et al. 1999, Astrophys. J., 517, 565\nSahoo P. K., Bishi B. K., Aygün S. 2018, New Astron., 60, 80\nSahoo P., Mishra B., Chakradhar G., Reddy D. 2014, Eur. Phys. J. Plus, 129, 49\nSahoo P. K., Mishra B. 2013, Int. J. Pure Appl. Math., 82, 87\nSetare M., Darabi F., 2012, Gen. Relativ. Gravit., 44, 2521\nSharif M., Yousaf Z. 2014, J. Cosmo. Astropart. Phys., 06\nSharif M., Zubair M. 2012, JCAP, 03028\nSotiriou T. P., Li B., Barrow J. D. 2011, Phys. Rev. D, 83, 104030\nTegmark M., Strauss M. A., Blanton M. R. et al. 2004, Phys. Rev. D, 69, 103501\nWeber F. 2005, Prog. Part. Nucl. Phys., 54, 193\nWei H., Ma X. P., Qi H. Y. 2011, Phys. Lett. B, 703, 74\nWitten E. 1984, Phys. Rev. D, 30, 272\nYılmaz İ., Baysal H., Aktaş C. 2012, Gen. Relativ. Gravit., 44, 2313",{"EN":386},"Contemporary piece of writing devotes to the investigation of plane symmetric cosmological model with quark and strange quark matter in the deformations of the Einstein’s theory of General Relativity (GR). At small or large scales (ultraviolet or infrared gravity), deformations of the Einstein’s theory could provide a better handling of cosmic acceleration without magnetism (along with singularities). In particular, a proper deformation of GR in the ultraviolet regime could play the role of describing the transition between GR and quantum gravity. As a matter of fact, although with a different purpose in mind, it was Einstein himself who proposed in the 30’s the reformulation of GR by taking the field of orthonormal frames or tetrads as the dynamical variable instead of the metric tensor (Einstein, Phys. Math. Kl 217, 401, 1928). As per the observation, pressure and energy density of the model approaches the bag constant in negative and positive ways at \n                  \n                    \n                  \n                  $$t\\rightarrow \\infty $$\n                  \n                    \n                  \n                , i.e. \n                  \n                    \n                  \n                  $$p\\rightarrow -B_c $$\n                  \n                    \n                  \n                 and \n                  \n                    \n                  \n                  $$\\rho \\rightarrow B_c $$\n                  \n                    \n                  \n                , the negative pressure due to the Dark Energy (DE) in the context of accelerated expansion of the universe. So the strange quark matter gives an idea of existence of dark energy in the universe and supports the observations of the SNe-I (Riess et al., Astron. J. 116,1009, 1998; Perlmutter et al., Astrophys. J. 517, 565, 1999). Also these results agree with the study of Aktas and Aygun (Chinese J. Phys. 55, 71, 2017) and Sahoo et al. (New. 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We use unsupervised machine learning methods to identify new members for nine nearby MW satellite galaxies using Gaia data release-3 (Gaia DR3) astrometry, the Dark Energy Survey (DES) and the DECam Local Volume Exploration Survey (DELVE) photometry. Two density-based clustering algorithms, DBSCAN and HDBSCAN, have been used in the four-dimensional astrometric parameter space (\n                \n                  \n                \n                $$\\alpha _{2016}$$\n                \n              , \n                \n                  \n                \n                $$\\delta _{2016}$$\n                \n              , \n                \n                  \n                \n                $$\\mu _{\\alpha } \\cos \\delta $$\n                \n              , \n                \n                  \n                \n                $$\\mu _\\delta $$\n                \n              ) to identify member stars belonging to MW satellite galaxies. Our results indicate that we can recover more than 80% of the known spectroscopically confirmed members in most satellite galaxies and also reject 95–100% of spectroscopic non-members. We have also added many new members using this method. We compare our results with previous studies using photometric and astrometric data and discuss the suitability of density-based clustering methods for MW satellite galaxies.",{"EN":612},"Possibilities of identifying members from Milky Way satellite galaxies using unsupervised machine learning algorithms",{"VOID":614},"10.1007\u002Fs12036-023-09990-4","https:\u002F\u002Flink.springer.com\u002Farticle\u002F10.1007\u002Fs12036-023-09990-4",[617,634,656,678],{"id":618,"sortIndex":103,"researcher":18,"roles":619,"affiliations":620,"properties":631},"555db3ab-e1f3-466e-a623-f0c0deff144a",[137],[621],{"id":18,"sortIndex":19,"affiliation":622,"properties":18},{"id":623,"createTime":624,"updateTime":625,"relativeEntities":626,"slug":627,"properties":628,"entityType":47,"verifyStatus":17,"verifyTime":18,"verifyNote":18,"syncStatus":17,"languages":18,"translateLanguages":18,"viewCount":19},"0f4e9790-160f-4d1a-b75f-60e15f57782d","2024-01-05T11:18:37.580+00:00","2024-09-21T06:07:17.013+00:00",[],"Department-of-Physics-Bangalore-University-Bangalore-India",{"title":629},{"VI":630},"Department of Physics, Bangalore University, Bangalore, India",{"title":632},{"VI":633},"Vijayakumar H. Doddamani",{"id":635,"sortIndex":19,"researcher":18,"roles":636,"affiliations":637,"properties":653},"0c3de012-7748-4cb0-8dec-7e6ee05b45af",[137],[638,646],{"id":18,"sortIndex":19,"affiliation":639,"properties":18},{"id":640,"createTime":641,"updateTime":641,"relativeEntities":642,"slug":18,"properties":643,"entityType":47,"verifyStatus":17,"verifyTime":18,"verifyNote":18,"syncStatus":17,"languages":18,"translateLanguages":18,"viewCount":19},"aaf0f01f-0859-46db-9b88-1b73de2a4ef3","2024-01-19T03:44:14.150+00:00",[],{"title":644},{"VI":645},"Indian Institute of Astrophysics, II Block, Koramangala, Bangalore, India",{"id":647,"sortIndex":106,"affiliation":648,"properties":652},"e439e9d0-49e7-48eb-ade9-2649f12e7d20",{"id":623,"createTime":624,"updateTime":625,"relativeEntities":649,"slug":627,"properties":650,"entityType":47,"verifyStatus":17,"verifyTime":18,"verifyNote":18,"syncStatus":17,"languages":18,"translateLanguages":18,"viewCount":19},[],{"title":651},{"VI":630},{},{"title":654},{"VI":655},"Devika K. 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A. 1974,ApJ,189, 101.",{"doi":868},"10.1086\u002F152776",{"id":18,"text":870,"url":18,"identifiers":871},"Stibbs, D. W. N. 1950,MNRAS,110, 395.",{"doi":872},"10.1093\u002Fmnras\u002F110.4.395",{"id":18,"text":874,"url":18,"identifiers":875},"Titus, J., Morgan, W. W. 1940,ApJ,92, 256.",{"doi":876},"10.1086\u002F144215",{"id":18,"text":878,"url":18,"identifiers":879},"Zhou, A.-Y. 2001,Communication in Asteroseismology,140, 59.",{},{"id":881,"createTime":882,"updateTime":883,"relativeEntities":884,"slug":885,"properties":886,"entityType":129,"verifyStatus":130,"verifyTime":883,"verifyNote":131,"syncStatus":17,"languages":18,"translateLanguages":18,"viewCount":19,"primaryUrl":895,"fullTextUrl":18,"authors":896,"publicationType":250,"publisherRelationship":927,"citationCount":18,"citationInfo":18,"publishDate":960,"publishYear":961,"citationAnalyzeStatus":17,"lastCitationAnalyze":18,"indexDatabases":18,"openAccess":18,"references":18,"isForceReanalyzing":286},"99de250f-7124-49f3-a0e3-a6774850b494","2023-12-12T19:41:21.742+00:00","2025-01-23T23:52:27.989+00:00",[],"HI-fluctuations-at-large-redshifts-II-the-signal-expected-for-the-GMRT",{"references":887,"abstract":889,"title":891,"doi":893},{"VOID":888},"Bharadwaj, S., Nath, B., Sethi, S. K. 2001,JApA. 22, 21.\nBharadwaj, S., Sethi, S. K. 2001,JApA,22, 293.\nBum, E. F., White, M. 1996,Astrophys. J.,460, 1071.\nEfstathiou, G., Bond, J. R., White, S. D. M. 1992,MNRAS, 250, 1p.\nLahav, O., Lilje, P. B., Primack, J. R., Rees, M., 1991,MNRAS,251, 128.\nLanzetta, K. M., Wolfe, A. M., Tumshek, D. A. 1995,Astrophys. J.,430, 435.\nPeebles, P. J. E. 1980,The Large-Scale Structure of the Universe (Princeton: Princeton University Press)\nPéroux, C, McMahon, R. G., Storrie-Lombardi, L. J., Irwin, M. J. 2001,MNRAS astroph\u002F0107045\nSaini, T., Bharadwaj, S., Sethi, K. S. 2001,Astrophys. J.,557, 421.\nStorrie-Lombardi, L. J., McMahon, R. G., Irwin, M. J. 1996,MNRAS,283, L79.\nSwarup, G., Ananthakrishan, S., Kapahi, V. K., Rao, A. P., Subrahmanya, C. R., Kulkarni, V. K.1991,Curr. Sci.,60, 95.",{"EN":890},"For the GMRT, we calculate the expected signal from red-shifted HI emission at two frequency bands centered at 610 and 325 MHz. The study focuses on the visibility-visibility cross-correlations, proposed earlier as the optimal statistical estimator for detecting and analyzing this signal. These correlations directly probe the power spectrum of density fluctuations at the redshift where the radiation originated, and thereby provide a method for studying the large scale structures at large redshifts. We present detailed estimates of the correlations expected between the visibilities measured at different baselines and frequencies. Analytic fitting formulas representing the salient features of the expected signal are also provided. These will be useful in planning observations and deciding an optimal strategy for detecting this signal.",{"EN":892},"HI fluctuations at large redshifts: II — the signal expected for the GMRT",{"VOID":894},"10.1007\u002FBF03012189","http:\u002F\u002Flink.springer.com\u002F10.1007\u002FBF03012189",[897,912],{"id":898,"sortIndex":19,"researcher":18,"roles":899,"affiliations":900,"properties":909},"f57fd74a-d4d8-4a80-8d8e-098281c39974",[137],[901],{"id":18,"sortIndex":19,"affiliation":902,"properties":18},{"id":903,"createTime":904,"updateTime":904,"relativeEntities":905,"slug":18,"properties":906,"entityType":47,"verifyStatus":17,"verifyTime":18,"verifyNote":18,"syncStatus":17,"languages":18,"translateLanguages":18,"viewCount":19},"bc9030b6-7ddf-4c0f-9e99-adba8e021983","2024-01-05T03:51:25.722+00:00",[],{"title":907},{"VI":908},"Department of Physics and Meteorology & Center for Theoretical Studies, I.I.T. Kharagpur, India",{"title":910},{"VI":911},"Somnath Bharadwaj",{"id":913,"sortIndex":106,"researcher":18,"roles":914,"affiliations":915,"properties":924},"0b29dc02-fd67-4544-a7a6-0a7fba70fb1b",[137],[916],{"id":18,"sortIndex":19,"affiliation":917,"properties":18},{"id":918,"createTime":919,"updateTime":919,"relativeEntities":920,"slug":18,"properties":921,"entityType":47,"verifyStatus":17,"verifyTime":18,"verifyNote":18,"syncStatus":17,"languages":18,"translateLanguages":18,"viewCount":19},"803ce24b-1897-402d-ad6d-831d8dd6a4f2","2023-12-12T19:41:34.461+00:00",[],{"title":922},{"VI":923},"Department of Mathematics, L.B.S. College, Gonda, India",{"title":925},{"VI":926},"Sanjay K. Pandey",{"url":895,"publisher":928,"properties":955},{"id":6,"createTime":7,"updateTime":8,"relativeEntities":929,"slug":10,"properties":930,"entityType":16,"verifyStatus":17,"verifyTime":18,"verifyNote":18,"syncStatus":17,"languages":18,"translateLanguages":18,"viewCount":19,"subjectFields":933,"manageAffiliations":934,"indexDatabases":935,"url":100,"thumbnailPath":18,"statistic":950,"gsStatistic":18,"type":109,"analyzePriority":18},[],{"issn":931,"title":932},{"VOID":13},{"EN":15},[],[],[936,943],{"id":63,"indexDatabase":937,"url":78,"indexYears":18,"academicFieldIds":942,"indexDatabaseRanking":18},{"id":65,"createTime":66,"updateTime":67,"relativeEntities":938,"label":939,"description":940,"key":74,"publicationTags":941,"standard":18},[],{"EN":70,"VI":70},{"VI":72,"EN":73},[76,77],[80],{"id":82,"indexDatabase":944,"url":95,"indexYears":96,"academicFieldIds":949,"indexDatabaseRanking":18},{"id":84,"createTime":85,"updateTime":86,"relativeEntities":945,"label":946,"description":947,"key":92,"publicationTags":948,"standard":18},[],{"EN":89,"VI":89},{"EN":89,"VI":91},[94],[98,99],{"impactFactor":19,"impactFactorByYear":951,"i10Index":19,"i10IndexLast5Year":19,"totalPublication":103,"totalPublicationByYear":952,"totalCitation":19,"totalCitationByYear":953,"totalCitationPerPublication":19,"totalCitationPerPublicationByYear":954,"hindexLast5Year":19,"hindex":19},{},{"2022":105,"2023":106},{},{},{"volume":956,"pages":958},{"VOID":957},"24",{"VOID":959},"23-35","2003-03-01",2003,{"id":963,"createTime":964,"updateTime":965,"relativeEntities":966,"slug":967,"properties":968,"entityType":129,"verifyStatus":130,"verifyTime":965,"verifyNote":131,"syncStatus":17,"languages":18,"translateLanguages":18,"viewCount":19,"primaryUrl":977,"fullTextUrl":18,"authors":978,"publicationType":250,"publisherRelationship":1067,"citationCount":18,"citationInfo":18,"publishDate":1100,"publishYear":1101,"citationAnalyzeStatus":17,"lastCitationAnalyze":18,"indexDatabases":18,"openAccess":18,"references":18,"isForceReanalyzing":286},"83b30ab8-dfaf-4d42-ae00-c96493105c04","2024-01-25T22:53:56.446+00:00","2025-02-14T23:51:43.943+00:00",[],"Stark-Broadening-Parameters-for-Neutral-Oxygen-Spectral-Lines",{"references":969,"abstract":971,"title":973,"doi":975},{"VOID":970},"Ben Nessib, N., Ben Lakhdar, Z., Sahal-Bréchot, S. 1996, Physica Scripta, 54, 608–613.\nBurke, P. G., Seaton, M. J. 1971, Meth. Comput. Phys., 10, 1–80.\nBurke, P. G., Hibbert, A., Robb, W. D. 1971, J. Phys. B, 4, 153–161.\nCowan, R. D. 1981, Theory of Atomic Structure and Spectra (Berkeley: Univ. California Press).\nCunto, W., Mendoza, C., Ochsenbein, F., Zeippen, C. J. 1993, Astron. Astrophys., 275, L5. Available: http:\u002F\u002Fcdsweb.u-strasbg.fr\u002Ftopbase\u002Ftopbase.html [2015, May 24].\nDubernet, M. L., Boudon, V., Culhane, J. L. . et al. 2010, JQSRT, 111, 2151–2159. http:\u002F\u002Fwww.vamdc.eu.\nGriem, H. R. 1974, Spectral line broadening by plasmas, Academic Press Inc., New York, USA and London, UK.\nKramida, A., Ralchenko, Yu., Reader, J., NIST ASD Team 2014, NIST Atomic Spectra Database (ver. 5.2), [Online]. Available: http:\u002F\u002Fphysics.nist.gov\u002Fasd [2015, May 24]. National Institute of Standards and Technology, Gaithersburg, MD.\nRixon, G., Dubernet, M. L., Piskunov, N. et al. 2011, VII International Conference on Atomic and Molecular Data and their Applications – ICAMDATA-2010 (AIP Conf. Proc. 1344, 107–115) (New York: Melville).\nRyabchikova, T., Piskunov, N., Kurucz, R. L., Stempels, H. C., Heiter, U., Pakhomov, Yu. Barklem, P. S. 2015, Physica Scripta, 90 (1–4), 054005.\nSahal-Bréchot, S. 1969, Astron. Astrophys., 1, 91–123.\nSahal-Bréchot, S. 1969, Astron. Astrophys., 2, 322–354.\nSahal-Bréchot, S. 1974, Astron. Astrophys., 35, 319–321.\nSahal-Bréchot, S., Dimitrijević, M. S. Ben Nessib, N. 2014, Atoms, 2, 225–252.\nSahal-Bréchot, S., Dimitrijević, M. S. Moreau, N. 2015, STARK-B database [online]. Available: http:\u002F\u002Fstark-b.obspm.fr [May 19, 2015]. Observatory of Paris, LERMA and Astronomical Observatory of Belgrade.\nSeaton, M. J. 1962, Proc. Phys. Soc., 79, 1105–1117.\nVennes, S., Kawka, A. Nemeth, P. 2011, MNRAS, 413, 2545–2553.",{"EN":972},"Stark broadening parameters for nine neutral oxygen (O I) lines have been determined within the impact approximation and the semiclassical perturbation method. The atomic data have been taken from the TOPbase and NIST atomic databases. The electron and proton Stark widths and shifts and ion broadening parameter values for these O I lines have been calculated for electron density of 10 16 cm −3 and for 4 different electron temperatures in the range of 5000 K to 40000 K. These Stark broadening parameters are compared with our previous results (Ben Nessib, N. et al.\n                        1996, Physica Scripta, 54, 603–613), where we calculated Stark broadening parameters for only four O I spectral lines and where Stark widths and shifts were compared with experimental and theoretical data available in the literature. In the present paper, we have also compared our results with the Griem’s book (Griem, H. R. 1974, Spectral line broadening by plasmas) and VALD (Ryabchikova, T. et al.\n                        2015, Physica Scripta, 90, 054005) values.",{"EN":974},"Stark Broadening Parameters for Neutral Oxygen Spectral Lines",{"VOID":976},"10.1007\u002Fs12036-015-9351-z","https:\u002F\u002Flink.springer.com\u002Farticle\u002F10.1007\u002Fs12036-015-9351-z",[979,994,1011,1023,1055],{"id":980,"sortIndex":103,"researcher":18,"roles":981,"affiliations":982,"properties":991},"dbcae2b8-15f6-4ea9-a466-5a14e6076a07",[137],[983],{"id":18,"sortIndex":19,"affiliation":984,"properties":18},{"id":985,"createTime":986,"updateTime":986,"relativeEntities":987,"slug":18,"properties":988,"entityType":47,"verifyStatus":17,"verifyTime":18,"verifyNote":18,"syncStatus":17,"languages":18,"translateLanguages":18,"viewCount":19},"509bf15e-c884-4c54-89ce-7c0e2d3858d9","2024-01-25T22:53:56.492+00:00",[],{"title":989},{"VI":990},"LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, Meudon Cedex, France",{"title":992},{"VI":993},"S. Sahal-Bréchot",{"id":995,"sortIndex":19,"researcher":18,"roles":996,"affiliations":997,"properties":1008},"51594b40-fd2e-412e-8947-c48907d693d8",[137],[998],{"id":18,"sortIndex":19,"affiliation":999,"properties":18},{"id":1000,"createTime":1001,"updateTime":1002,"relativeEntities":1003,"slug":1004,"properties":1005,"entityType":47,"verifyStatus":17,"verifyTime":18,"verifyNote":18,"syncStatus":17,"languages":18,"translateLanguages":18,"viewCount":19},"1548f521-61cd-4fbb-ac4d-a4b22a9be7c3","2024-01-11T05:03:35.224+00:00","2024-10-14T16:17:06.176+00:00",[],"Department-of-Physics-and-Astronomy-College-of-Science-King-Saud-University-Riyadh-Saudi-Arabia",{"title":1006},{"VI":1007},"Department of Physics and Astronomy College of Science, King Saud University, Riyadh, Saudi Arabia",{"title":1009},{"VI":1010},"N. Alonizan",{"id":1012,"sortIndex":106,"researcher":18,"roles":1013,"affiliations":1014,"properties":1020},"a000abf7-8252-48c5-bf7d-1096fa5eb7b5",[137],[1015],{"id":18,"sortIndex":19,"affiliation":1016,"properties":18},{"id":1000,"createTime":1001,"updateTime":1002,"relativeEntities":1017,"slug":1004,"properties":1018,"entityType":47,"verifyStatus":17,"verifyTime":18,"verifyNote":18,"syncStatus":17,"languages":18,"translateLanguages":18,"viewCount":19},[],{"title":1019},{"VI":1007},{"title":1021},{"VI":1022},"R. Qindeel",{"id":1024,"sortIndex":48,"researcher":18,"roles":1025,"affiliations":1026,"properties":1052},"02a12f23-1629-45b2-a945-f8df2fb06558",[137],[1027,1032,1042],{"id":18,"sortIndex":19,"affiliation":1028,"properties":18},{"id":985,"createTime":986,"updateTime":986,"relativeEntities":1029,"slug":18,"properties":1030,"entityType":47,"verifyStatus":17,"verifyTime":18,"verifyNote":18,"syncStatus":17,"languages":18,"translateLanguages":18,"viewCount":19},[],{"title":1031},{"VI":990},{"id":1033,"sortIndex":106,"affiliation":1034,"properties":1041},"d596cfbf-f8d0-49a9-beba-041551f40233",{"id":1035,"createTime":1036,"updateTime":1036,"relativeEntities":1037,"slug":18,"properties":1038,"entityType":47,"verifyStatus":17,"verifyTime":18,"verifyNote":18,"syncStatus":17,"languages":18,"translateLanguages":18,"viewCount":19},"ce1937cc-bb14-4436-b53b-a1b2a4ecb07d","2023-12-13T10:02:45.877+00:00",[],{"title":1039},{"VI":1040},"Astronomical Observatory, Belgrade, Serbia",{},{"id":1043,"sortIndex":105,"affiliation":1044,"properties":1051},"c9ba3c6e-30f3-4bbc-a3cc-f0af843a8f4e",{"id":1045,"createTime":1046,"updateTime":1046,"relativeEntities":1047,"slug":18,"properties":1048,"entityType":47,"verifyStatus":17,"verifyTime":18,"verifyNote":18,"syncStatus":17,"languages":18,"translateLanguages":18,"viewCount":19},"d5774f71-0763-4574-b787-b3cb17c87022","2024-01-25T22:53:56.514+00:00",[],{"title":1049},{"VI":1050},"IHIS Techno Experts, Belgrade-Zemun, Serbia",{},{"title":1053},{"VI":1054},"Milan S. Dimitrijević",{"id":1056,"sortIndex":105,"researcher":18,"roles":1057,"affiliations":1058,"properties":1064},"9dbe675e-ead2-4fbd-8868-dcbaa177c99f",[137],[1059],{"id":18,"sortIndex":19,"affiliation":1060,"properties":18},{"id":1000,"createTime":1001,"updateTime":1002,"relativeEntities":1061,"slug":1004,"properties":1062,"entityType":47,"verifyStatus":17,"verifyTime":18,"verifyNote":18,"syncStatus":17,"languages":18,"translateLanguages":18,"viewCount":19},[],{"title":1063},{"VI":1007},{"title":1065},{"VI":1066},"N. Ben Nessib",{"url":977,"publisher":1068,"properties":1095},{"id":6,"createTime":7,"updateTime":8,"relativeEntities":1069,"slug":10,"properties":1070,"entityType":16,"verifyStatus":17,"verifyTime":18,"verifyNote":18,"syncStatus":17,"languages":18,"translateLanguages":18,"viewCount":19,"subjectFields":1073,"manageAffiliations":1074,"indexDatabases":1075,"url":100,"thumbnailPath":18,"statistic":1090,"gsStatistic":18,"type":109,"analyzePriority":18},[],{"issn":1071,"title":1072},{"VOID":13},{"EN":15},[],[],[1076,1083],{"id":63,"indexDatabase":1077,"url":78,"indexYears":18,"academicFieldIds":1082,"indexDatabaseRanking":18},{"id":65,"createTime":66,"updateTime":67,"relativeEntities":1078,"label":1079,"description":1080,"key":74,"publicationTags":1081,"standard":18},[],{"EN":70,"VI":70},{"VI":72,"EN":73},[76,77],[80],{"id":82,"indexDatabase":1084,"url":95,"indexYears":96,"academicFieldIds":1089,"indexDatabaseRanking":18},{"id":84,"createTime":85,"updateTime":86,"relativeEntities":1085,"label":1086,"description":1087,"key":92,"publicationTags":1088,"standard":18},[],{"EN":89,"VI":89},{"EN":89,"VI":91},[94],[98,99],{"impactFactor":19,"impactFactorByYear":1091,"i10Index":19,"i10IndexLast5Year":19,"totalPublication":103,"totalPublicationByYear":1092,"totalCitation":19,"totalCitationByYear":1093,"totalCitationPerPublication":19,"totalCitationPerPublicationByYear":1094,"hindexLast5Year":19,"hindex":19},{},{"2022":105,"2023":106},{},{},{"volume":1096,"pages":1098},{"VOID":1097},"36",{"VOID":1099},"661-669","2015-12-16",2015,{"id":1103,"createTime":1104,"updateTime":1105,"relativeEntities":1106,"slug":1107,"properties":1108,"entityType":129,"verifyStatus":130,"verifyTime":1117,"verifyNote":131,"syncStatus":17,"languages":18,"translateLanguages":18,"viewCount":19,"primaryUrl":1118,"fullTextUrl":18,"authors":1119,"publicationType":250,"publisherRelationship":1176,"citationCount":18,"citationInfo":18,"publishDate":1209,"publishYear":1210,"citationAnalyzeStatus":17,"lastCitationAnalyze":18,"indexDatabases":18,"openAccess":18,"references":18,"isForceReanalyzing":286},"9204055b-eb62-42d6-a0e4-0a0e4b9fcca2","2023-12-06T12:57:20.993+00:00","2025-01-23T23:51:24.493+00:00",[],"Distribution-of-latitudes-and-speeds-of-Coronal-Mass-Ejections-in-the-northern-and-southern-hemispheres-in-cycle-23",{"references":1109,"abstract":1111,"title":1113,"doi":1115},{"VOID":1110},"Abramenko, V. I., Yurchyshyn, V. B., Wang, H., Spirock, T. J., Goode, P. R. 2003, ApJ, 597, 1135.\nAoki, S. I., Yashiro, S., Shibata, K. 2003, In: Proc. 28th Int. Cosmic Ray Conf. (eds) T. Kajita et al. (Japan) 2729.\nAtaç, T., Özgüç, A. 1996, Solar Phys., 166, 201.\nAtaç, T., Özgüç, A. 1998, Solar Phys., 180, 397.\nCane, H. V., Richardson, I. G. 2003, JGR, 108, A4, 1156.\nGopalswamy, N., Lara, A., Lepping, R. P., Kaiser, M. L., Berdichevsky, D., St. Cry, O. C. 2000, GRL, 27, 145.\nGopalswamy, N., Lara, A., Yashiro, S., Kaiser, M. L., Howard, R. A. 2001, JGR, 106, 29207.\nGopalswamy, N., Lara, A., Yashiro, S., Howard, R. A. 2003, ApJ, 598, L63.\nHarvey, K. L., White, O. R. 1999, JGR, 104, 19759.\nHaber, D. A., Hindman, B. H., Toomer, J. 2002, ApJ, 570, 855.\nHoward, R. A., Sheeley, Jr. N. R., Koomen, M. J., Michels, D. J. 1985, JGR, 90, 8173.\nHundhausen, A. J. 1993, JGR, 98, 13177.\nHundhausen, A. J., Burkepile, J. T., St. Cry, O. C. 1994, JGR, 99, 6543.\nJiang, J., Chatterjee, P., Choudhuri, A. R. 2007, MNRAS, 381, 1527.\nKaufmann, P., Gimenez de Castro, C. G., Makhmutov, V. S., Raulin, J.-P., Schwenn, R., Levato, H., Rovira, M. 2003, JGR, 108, 1280.\nLeblanc, Y., Dulk, G. A., Vourlidas, A., Bougeret, J. L. 2001, JGR, 106, 25301.\nLi, K. J., Schmieder, B., Li, Q.-Sh. 1998, Astron. Astrophys. Suppl. Ser., 131, 99.\nLi, K. J., Wang, J. X., Xiong, S. Y., Liang, H. F., Yun, H. S., Gu, X. M. 2000, A&A, 383, 648.\nLi, K. J., Irie, M., Wang, J. X., Xiong, S. Y., Yun, H. S., Liang, H. F., Zhan, L. S., Zhao, H. J. 2002, PASJ, 54, 787.\nLi, K. J., Wang, J. X., Zhan, L. S., Yun, H. S., Liang, H. F., Zhao, H. J., Gu, X. M. 2003, Solar Phys., 215, 99.\nLiu, H. L. 1996, Tong Ji Xue Jiao Cheng, Shanghai: Shanghai Finance Univ. Press.\nMichalek, G., Gopalswamy, N., Lara, A., Manoharan, P. K. 2004, A&A, 423, 729.\nTousey, R. 1973, The solar corona, In: Space Research XIII (eds) Rocroft, M. J., Runcorn, S. K. (publishers, Akademie-Verlag, Berlin) 713.\nWang, Y. M., Ye, P. Z., Wang, S., Zhou, G. P., Wang, J. X. 2002, JGR, 107, A11, 1340.\nWaldmeier, M. 1971, Solar Phys., 20, 332.\nYashiro, S., Gopalswamy, N., Michalek, G., St. Cry, O. C., Plunkett, S. P., Rich, N. B., Howard, R. A. 2004, JGR, 109, A07105.\nYeh, Chin-teh, Ding, M. D., Chen, P. F. 2005, Solar Phys., 229, 313.\nYurchyshyn, V., Yashiro, S., Abramenko, V., Wang, H., Gopalswamy, N. 2005, ApJ, 619, 599.\nZhang, J., Dere, K. P. 2006, ApJ, 649, 1100.\nZhao, J. W., Kosovichev, A. G. 2004, ApJ, 603, 776.\nZhou, G. P., Wang, J. X., Zhang, J. 2006, A&A, 445, 1133.",{"EN":1112},"Distribution of latitudes and speeds of Coronal Mass Ejections (CMEs) in the northern and southern hemispheres in cycle 23, from September 1996 to December 2006, have been analyzed. By calculating the actual probability of the hemispheric distribution of the activity of the CME, we find that a southern dominance of the activity of the CME is shown to occur in cycle 23 from September 1996 to December 2006. The CME activity occurs at all latitudes and is most common at low latitudes. This should furnish evidence to support that CMEs are associated with source magnetic structures on a large spatial scale, even with transequatorial source magnetic structures on a large spatial scale. The latitudinal distribution of CMEs in the northern and southern hemispheres are no different from a statistical point of view. The speed distribution in the northern and southern hemispheres are nearly identical and to a good approximation they can be fitted with a single lognormal distribution. This finding implies that, statistically, there is no physical distinction between the CME events in the southern and northern hemispheres and the same mechanism of a nonlinear nature acting in both the CME events in the northern and southern hemispheres. Our conclusions seem to suggest that the northern-southern asymmetry of the CME events is related to the northern-southern asymmetry in solar dynamo theory (Jiang et al. 2007).",{"EN":1114},"Distribution of latitudes and speeds of Coronal Mass Ejections in the northern and southern hemispheres in cycle 23",{"VOID":1116},"10.1007\u002Fs12036-007-0018-2","2025-01-23T23:51:24.492+00:00","http:\u002F\u002Flink.springer.com\u002F10.1007\u002Fs12036-007-0018-2",[1120,1145,1157],{"id":1121,"sortIndex":19,"researcher":18,"roles":1122,"affiliations":1123,"properties":1142},"c51c54b4-04d6-486e-b54b-e5e0f785b525",[137],[1124,1134],{"id":1125,"sortIndex":106,"affiliation":1126,"properties":1133},"b3b07a62-0a41-4f9b-b6f8-87efa489f536",{"id":1127,"createTime":1128,"updateTime":1128,"relativeEntities":1129,"slug":18,"properties":1130,"entityType":47,"verifyStatus":17,"verifyTime":18,"verifyNote":18,"syncStatus":17,"languages":18,"translateLanguages":18,"viewCount":19},"f539743d-2ba4-4719-81fb-379c3b47c535","2023-12-06T12:57:14.480+00:00",[],{"title":1131},{"VI":1132},"School of Graduate, CAS, Beijing, China",{},{"id":18,"sortIndex":19,"affiliation":1135,"properties":18},{"id":1136,"createTime":1137,"updateTime":1137,"relativeEntities":1138,"slug":18,"properties":1139,"entityType":47,"verifyStatus":17,"verifyTime":18,"verifyNote":18,"syncStatus":17,"languages":18,"translateLanguages":18,"viewCount":19},"cf7cddab-bec4-418a-82f8-cb4210646014","2023-12-06T12:57:21.005+00:00",[],{"title":1140},{"VI":1141},"National Astronomical Observatories\u002FYunnan Observatory, CAS, Kunming, China",{"title":1143},{"VI":1144},"P. 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J. 1982,Astrophys. J.,255, 245.",{"doi":1302},"10.1086\u002F159824",{"id":18,"text":1304,"url":18,"identifiers":1305},"Arnett, W. D. 1969,Astrophys. Space Sci.,5, 180.",{"doi":1306},"10.1007\u002FBF00650291",{"id":18,"text":1308,"url":18,"identifiers":1309},"Arnett, W. D. 1978,Astrophys. J.,219, 1008 (A78).",{"doi":1310},"10.1086\u002F155865",{"id":18,"text":1312,"url":18,"identifiers":1313},"Arnett, W. D. 1979,Astrophys. J.,230, L37.",{"doi":1314},"10.1086\u002F182957",{"id":18,"text":1316,"url":18,"identifiers":1317},"Arnett, W. D., Thielemann, F.-K. 1984, inStellar Nucleosynthesis, Eds C. Chiosi & A. Renzini, D. Reidel, Dordrecht, p. 145.",{"doi":1318},"10.1007\u002F978-94-009-6348-1_13",{"id":18,"text":1320,"url":18,"identifiers":1321},"Audouze, J., Tinsley, B. M. 1976,A Rev. Astr. Astrophys.,14, 43.",{"doi":1322},"10.1146\u002Fannurev.aa.14.090176.000355",{"id":18,"text":1324,"url":18,"identifiers":1325},"Bisiacchi, G. F., Firmani, C., Sarmiento, A. F. 1983,Astr. Astrophys.,119, 167.",{},{"id":18,"text":1327,"url":18,"identifiers":1328},"Cameron, A. G. W. 1973, inExplosive Nucleosynthesis, Eds D. N. Schramm & W. D. Arnett, Univ. Texas Press, p. 3.",{},{"id":18,"text":1330,"url":18,"identifiers":1331},"Chiosi, C. 1979,Astr. Astrophys.,80, 252.",{},{"id":18,"text":1333,"url":18,"identifiers":1334},"Chiosi, C., Caimmi, R. 1979,Astr. Astrophys.,80, 234.",{},{"id":18,"text":1336,"url":18,"identifiers":1337},"Clegg, R. E. S. 1977,Mon. Not. R. Astr. Soc,181, 1.",{"doi":1338},"10.1093\u002Fmnras\u002F181.1.1",{"id":18,"text":1340,"url":18,"identifiers":1341},"Clegg, R. E. S., Lambert, D. L., Tomkin, J. 1981,Astrophys. J.,250, 262.",{"doi":1342},"10.1086\u002F159371",{"id":18,"text":1344,"url":18,"identifiers":1345},"Colgate, S. A., Petschek, A. G. 1980 inType I Supernovae, Ed. J. C. Wheeler, Univ. Texas, p. 42.",{},{"id":18,"text":1347,"url":18,"identifiers":1348},"French, H. B. 1983,Astrophys. J.,273, 214.",{"doi":1349},"10.1086\u002F161360",{"id":18,"text":1351,"url":18,"identifiers":1352},"Garmany, C. D., Conti, P. S., Chiosi, C. 1982,Astrophys. J.,263, 777.",{"doi":1353},"10.1086\u002F160548",{"id":18,"text":1355,"url":18,"identifiers":1356},"Gingold, R. A. 1977,Mon. Not. R. Astr. Soc.,178, 569.",{"doi":1357},"10.1093\u002Fmnras\u002F178.4.569",{"id":18,"text":1359,"url":18,"identifiers":1360},"Hacyan, S., Dultzin-Hacyan, D., Torres-Peimbert, S., Peimbert, M. 1976,Rev. Mex. Astr. Astrofis.,1, 355.",{},{"id":18,"text":1362,"url":18,"identifiers":1363},"Humphreys, R. M., McElroy, D. B. 1984,Astrophys. J.,284, 565.",{"doi":1364},"10.1086\u002F162439",{"id":18,"text":1366,"url":18,"identifiers":1367},"Iben, I. Jr., 1981, inEffects of Mass loss on Stellar Evolution, Eds C. Chiosi & R. Stalio, D. Reidel, Dordrecht, p. 373.",{"doi":1368},"10.1007\u002F978-94-009-8500-1_55",{"id":18,"text":1370,"url":18,"identifiers":1371},"Iben, I. Jr., Truran, J. W. 1978,Astrophys. 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J.,255, 1.",{"doi":1435},"10.1086\u002F159796",{"id":18,"text":1437,"url":18,"identifiers":1438},"Renzini, A., Voli, M. 1981,Astr. Astrophys.,94, 175.",{},{"id":18,"text":1440,"url":18,"identifiers":1441},"Romanishin, W., Angel, J. R. P. 1980,Astrophys. J.,235, 992.",{"doi":1442},"10.1086\u002F157704",{"id":18,"text":1444,"url":18,"identifiers":1445},"Shaver, P. A., McGee, R. X., Newton, L. M., Danks, A. C., Pottasch, S. R. 1983,Mon. Not. R. astr. Soc.,204, 53.",{"doi":1446},"10.1093\u002Fmnras\u002F204.1.53",{"id":18,"text":1448,"url":18,"identifiers":1449},"Sneden, C., Lambert, D. L., Whitaker, R. W. 1979,Astrophys. J.,234, 964.",{"doi":1450},"10.1086\u002F157580",{"id":18,"text":1452,"url":18,"identifiers":1453},"Sutherland, P. G., Wheeler, J. C. 1984,Astrophys. J.,280, 282.",{"doi":1454},"10.1086\u002F161995",{"id":18,"text":1456,"url":18,"identifiers":1457},"Tammann, G. A. 1982, inSupernovae: A Survey of Current Research, Eds M. J. Rees & R. J. Stoneham, D. Reidel, Dordrecht, p. 371.",{"doi":1458},"10.1007\u002F978-94-009-7876-8_23",{"id":18,"text":1460,"url":18,"identifiers":1461},"Tinsley, B. M. 1977a,Astrophys. J.,216, 548.",{"doi":1462},"10.1086\u002F155496",{"id":18,"text":1464,"url":18,"identifiers":1465},"Tinsley, B. M. 1977b, inSupernovae, Ed. D. N. Schramm, D. Reidel, Dordrecht, p. 117.",{"doi":1466},"10.1007\u002F978-94-010-1229-4_11",{"id":18,"text":1468,"url":18,"identifiers":1469},"Tinsley, B. M. 1979,Astrophys. J.,229, 1046.",{"doi":1470},"10.1086\u002F157039",{"id":18,"text":1472,"url":18,"identifiers":1473},"Tinsley, B. M. 1980a,Fundam. Cosmic Phys.,5, 287.",{},{"id":18,"text":1475,"url":18,"identifiers":1476},"Tinsley, B. M. 1980b,Astr. Astrophys.,89, 246.",{},{"id":18,"text":1478,"url":18,"identifiers":1479},"Torres-Peimbert, S. 1984, inStellar Nucleosynthesis, Eds C. Chiosi & A. Renzini, D. Reidel, Dordrecht, p. 3.",{"doi":1480},"10.1007\u002F978-94-009-6348-1_1",{"id":18,"text":1482,"url":18,"identifiers":1483},"Twarog, B. A. 1980,Astrophys. J.,242, 242.",{"doi":1484},"10.1086\u002F158460",{"id":18,"text":1486,"url":18,"identifiers":1487},"Twarog, B. A., Wheeler, J. C. 1982,Astrophys. J.,261, 636 (TW).",{"doi":1488},"10.1086\u002F160375",{"id":18,"text":1490,"url":18,"identifiers":1491},"Weidemann, V. 1977,Astr. Astrophys.,59, 411.",{},{"id":18,"text":1493,"url":18,"identifiers":1494},"Weidemann, V., Koester, D. 1983,Astr. Astrophys.,121, 77.",{},{"id":18,"text":1496,"url":18,"identifiers":1497},"Wheeler, J. C. 1978,Mem. Soc. astr. Ital.,49, 349.",{},{"id":18,"text":1499,"url":18,"identifiers":1500},"Wheeler, J. C. 1981,Rep. Prog. Phys.,44, 85.",{"doi":1501},"10.1088\u002F0034-4885\u002F44\u002F2\u002F001",{"id":18,"text":1503,"url":18,"identifiers":1504},"Wheeler, J. C., Miller, G. E., Scalo, J. M. 1980,Astr. Astrophys. 82, 152 (WMS).",{},{"id":18,"text":1506,"url":18,"identifiers":1507},"Woosley, S. E., Axelrod, T. S., Weaver, T. A. 1984, inStellar Nucleosynthesis, Ed. C. Chiosi & A. Renzini, D. Reidel, Dordrecht, p. 263.",{"doi":1508},"10.1007\u002F978-94-009-6348-1_22",{"id":18,"text":1510,"url":18,"identifiers":1511},"Woltjer, L. 1984, inProc. Workshop Supernovae, their Progenitors and Remnants, Eds V. Radhakrishnan & G. Srinivasan, Indian Acad. Sci., Bangalore (in press).",{},{"id":18,"text":1513,"url":18,"identifiers":1514},"Wu, C-C., Leventhal, M., Sarazin, C. L., Gull, T. R. 1983,Astrophys. J.,269, L5.",{"doi":1515},"10.1086\u002F184044"]