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Scientometric Portrait of Nobel Laureate S. Chandrasekhar

B.S. Kademani, V. L. Kalyane and A. B. Kademani

S. ChandntS.ekhar, the well Imown Astrophysicist is wide!)' recognised as a ver:' successful Scientist. His publications \\'ere analysed by year"domain, collaboration pattern, d:lannels of commWtications used, keywords etc. The results indicate that the temporaJ ,'ari;.&-tjon of his productivit." and of the t."pes of papers p,ublished by him is of sudt a nature that he is eminent!)' qualified to be a role model for die y6J;mf;ergene-ration to emulate. By the end of 1990, he had to his credit 91 papers in StelJJlrSlructllre and Stellar atmosphere,f. 80 papers in Radiative transfer and negative ion of hydrogen, 71 papers in Stochastic, ,ftatisticql hydromagnetic problems in ph}'sics and a,ftrono"9., 11 papers in Pla.fma Physics, 43 papers in Hydromagnetic and ~}.droa:rnamic ,S"tabiJjty,42 papers in -virial theorem, 83 papers in Relativi,ftic a.ftrophy,fic.f, 61 papers in Malhematical theory. of Black hole,f and coUoiding waves, and 19 papers of genual interest. The higb~t Collaboration Coefficient \\'as 0.5 during 1983-87. Producti"it." coefficient ,,.as 0.46. The mean Synchronous self citation rate in his publications \\.as 24.44. Publication densi~. \\.as 7.37 and Publication concentration \\.as 4.34. Ke.}.word.f/De,fcriptors: Biobibliometrics; Scientometrics; Bibliome'trics; Collaboration; lndn.idual Scientist; Scientometric portrait; Sociolo~' of Science, Histor:. of St.-iencc.

1. Introduction his three undergraduate years at the Institute for Subrahmanvan Chandrasekhar ,,.as born in Theoretisk Fysik in Copenhagen. L.1:bore (then a part 'of British India) on 19 October He ,,as a",arded Ph. D. degree by Cariibridge 1q i O He had his earl;. education b;.' pri,.ate tution Universit~. in 1933. He ,vas elected as a fello,\' at till hc \\"as t\\"el\'e. He had his high school education Trinit~. College forthc period 1933-37. He ,vas a in t11eHindu High School. Triplicane during the Rescarch Associate at Ycrkes Obser,~to~'. .-\.~~rs 1922-25. He had his Unive~it\. education at Chicago during 1936-38. He becamc Assistant rhe Presidenc:. College during 1925-30 and Protcssor. Chicago Universit~. during 1938-41. , recei\.ed his Bachelor's deg.Tee. B.Sc.(Hon.). in Associate Professor (1942-43), Professor (1943-, ph:'sics in June 1930. He was a\\"arded a 47). Distinguished Service Professor of Theoretical Govt:rnment of India Scholarship for gradu:lte Astroph~.sics ( 194 7~52), Morton D. Hull studil.'s in Cambridge" England in Jul:. 1930 to \\"ork Distinguishcd Servicc Profcssor of Theoretical in thl.'orctical ph~.sics. mort: specifica1I~. in tht: Astroph~sics ( 1952-19X6 ). Hc ,,.as Professor tht:o~ of stcll~r structurl.:. thc ficld \\"hic1J \\":15. Eml:ritus ( IlJ86-95). Hc dicd of hcart !ailurc in domill3tcd th~n b~. Arthur Eddington. Chicago o!12lst August 1995. Ht: bt:camt: a research studcn! undcr thc Hc ,vas an cditor ofthc .ioumal Astroph.\"lsical supcr\'ision of professor R. H. Fowler (\\"ho was .Journal during 1952 -1971. When hc took over, responsible for his admission to Trinity College). thc.ioumal was nothing more than a private journal On the ad\'ice ofProfessor P. A. M. Dirac, he spent of Chicago University .By the time he resigned it

JISSJ .2(2-3) June -September 1996 llq KADEMANI. KAL y ANE AND KADEMANI had becomc .Ul official .jollmal of thc Amcric~l imprcssion on )'oung CbaJldrasckhar.s mind,1l1is pcrhaps \\'as rcsponsiblc for his taking up research Astronomical S6cict).. in the fil;;ld of aJ1dAstrophysics, . 'nlerc is no doubt. th;ll hl.: \\'as il1tlul.:ncl.:d by his illustrious ul1clc Sir C. V. Ramali the Nobel ChaJldrasekhar's contribution is particularl~' Laurc~tc tor IlJ30 \,cll kl1o\,n for his i\1vl;ntion on multi-facctcd and covcrs many aspects of thl.: Raman E;(fect . evolution ofstarso An important part ofhis work Man~. honours .u1d :l\v~rds were bcsto\Vcd on is a study concerning the problems ofstabilit)' in him in rccognitiol1 ofhis contribution in thc ficld diffcrl.:nt phascs ofthcir cvolution, He has studil.:d of Astroph~.sics Import:ult oncsbcil1g . rclativi~lic I.:ffccts. \vllicil bCC~1111Cilll"ort~\Ilt I. Fcllo\, oftl1l.' Ro~.al Socil.:t~' ofLol1dol1- Il)44 bI.:C~lUSI.:of till.: I.:xtrl.:llll.: conditions \vhiciI ~lriSI.: 2. Ad.ullS prizl.: (C.U\1bridgc Univcrsit~.) -1947. during thl.: latcr stagl.:S of thl.: .s dl.:vl.:lopllll.:nt, One of Chandrasckhar.s most well kno\\'n 3. Brucc Medal of thc Astronomical Socicty of contributions i~ his stud)' of the S'lntc/ltre (~rWhile the Pacific -1952. Dwa,:-f\', In rccent ycars hc had worked on lhe 4. Gold Mcd:ll ofthc Ro~'~1lAstronomic."11 Socict~. Ma/hematical Theury ~fBlack Hule,\', ofLondon -1952. His books: An Jntrodu,,'ti(m tu th(.' Study (II 5. Electcd to tI,C N:ltiul1al Acadcmy of Scicncl.:s - St(.'llar ,\'tr/tctur(.' (1<.)39); Prin(.'iples ufStellar 1955. J).j,'numi(.'s ( 1942): J~adiative, Tran.\:f'er ( 1950): 6. Rumtord Medal ofthe American AcaLlcmy of Plasma Ph)'si(.'s ( 1960); Hydrodynal11i(.' aJqd Arts ~ld Scicl1ccs -1957. H.\.'dr()magneti(.' Stability (1961); 1~llips()idul 7, Sriniv;ts~ Ram:ll1u.ian Mcd~l of tllC 111di:l11 j;oi}!,/tr(.'s of [~'Iuilibrium ( 1969); and 1'h(.' N~tiol1;t1 Scicl1cc Ac~dcmy -1962. Mathema/icaI7nef)ry (~fBlack Holes () 9K3 ) havc 8, Ro~.al Mcdal ofthc Ro~'al Socjcty -1962. becomc classics in thc fields of Astronomy aJld 9. N~tiol1al Mcd~1 of Sci~ncl; (Unitcd St~tl;.S) - Spacc rcscarch, 1968 Hc had wide intcrest in music and litt:raturc. 10. Padma VibhllS~l Titlc (lndja) -196~. aJ1d ht: \vrotc a book t:ntitlcd Truth and h(.'au/}' II. Henl")' Drnpcr Mcdal ofthc Nation:ll Acadcmy aestlleti(..s a)1d m()tivations in scienc(.' , His filIal of Sci~l1cl.:s -1971. Smolucho\Vski Mcdal book was a comml.:ntary on, Newt()n .s principia (Polish Ph~.sic:ll Socict~'). ,t()r Ih(.' cummun reader, published early 1995, 12. DaIU1ie Heil1cm~ln Prizc of Americ~l Ph~'sic.'1l Chandrasckhar had to facc sevcral Societ~. -1974. humiliating cxpcricnccs in the hands of notcd 13. Nobcl Prizc -IlJX3. astronoml.:rs \\'hich did not daJ11pCnhis zcal, spirit 14. Dr. Tomalla Prizc (E.rH. Zurich). aJld scicntific tempcr which was in him by birth, It is notcworthy to mcntion that 15. Coplc~. M~dal of RO~~11Socil,:t~' -llJX4. ChaJldrasckhar.s studcnts Tsung -Dao Lec ~d 16. R. D. Birla A\\:lrd -Il)X4. , Chcn Ning YaJlg wl.:rc awardcd Nobcl prizl.: in 17, Vo"lil1l1B:lppll Mcdal uf thl; Il1di~l N:ltiol1al physics tor 1957 at thcir agc 31 aJld 35 rcspcctivt:ly Scicl1cc Acadl.:m\" -II.)X.' . for thcir ill\'cstigation ofthl.: so-calll.:d parity la\vs Hc \\as ~1lso :I ml.:mbcr of follo\\il1g which Icd to thl.: disco\'crics rcgarding elemcntar)' Academics : particles, S, Challdrasckhar \vas awarded Nobel Nation~1 Ac:ldc.:m~. ofScicnccs prize jointly \\'ith A, Fo\v~cr for his contributions Amcric~l Acau~m). of Arts:lnd Scicl1cl.:s on thc c\'olution of in 19K3 when he was 73 ~'I.:..rsof agl.: mainly for his wcll known discovcr)' Ro~'al AstroI1O1nil..:11Socict~. .Ch~uldrasckhar limit. n;t1lll.:daftcr him which statcs Amcric~ul ,\strol1omical Socict~' that S(i"l(.' slars ar(.' I()() massive t() b(.'come white Royal Socict~. ,hra,:-t:\'tar which i~.,torn,(.'d with mas.l' gr(.'ater than As a studci1l Ch~1l1drasckhar had rccl:j ...l.:d:1S ~ a li'"itin,1,' value (1.-1 !vf.,), prize, Eddil1gtol1.s tamolls book Th£: Int(.'rnal -n}1.:Nobel prize is rcgardcd not only by laymcn Constillltj()n ()I. till: .)(al'.~. \vhich Icft :l lastil1g but also by scientists as thc most honorific

120 JISSJ. 2(2-3} June .,September 1996 SCIENTO1'v1ETRICPORTRAIT OF NOBEL LAUREA TE S. CHAN~RASEKHAR

recognition of scientific achievenlent. The prestige ofd1e first \\:rite~ to suggest scientific publication ofthc Nobel prize is so great that it enhances tile as a measure of research productivity was Nobel standing of nations and institutions as well as the LaureareWilliam Shokley [12] \\-ho was interested reputation ofits laurea[e.'i [ 1-3]. His \\.orks have in measuring research.productivity among ~ \\ell documented [4-9]. indi\ridual \vithin a group by analysing their Citation anal~.sis of some important publications. A few Studies have been recentl~' conm"burions of S. Chandrasekhar has aIread~. published on individual scientiSts [10,13-4-1]. been carried out [ 101. This stud~. deals with six Bibliographic details of the publications ofS. citarionclassjcs ,\"hich have been identified based Chandrnsekhar were documented on cards from on the citations received to the papers of S. the list appended at the end of volume six of Chandrasekhar. These six papers received 53% of Selected papers of S. Chandrasekhar [42] and tora1 ) 0,359 citations during the period under stud). sorting \vas done as per requirements of the study. and concluded that there is a high correlation in Normal count procedure [43] was followed. quanrit)', qualit." of,vorks. citedness anareceiving Ftil1 credit was given to each ~thor regardless of honours and a,\'ards . whether he happensto be the first or the last author. It is \\,idely recognised that scientists allover the 2. Objectives world look at their O\\'Dpapers exclusively in that Objectives of present work are to highlight wa)'. Similarly titles 'of the articles were analysed quantitative aspects of the research and one score was alloted for each ke)"vord, communications : sub.je~,joumal, etc. The degreeof collabornnon [44] in a discipline (a) authorship pattern, was defined as the ratio of the number of (b) domainwise contribution, collaborative research papers to the total nl;lmber (c) authorproductivi1.", of researchpapers published in the discipline during (d) use of channels of communication a certain period of time (Figure 3). (e) bibliographic characteristics of publications, Vinkler [45] defined (Table -3) Publication and Densit). as the ratio of the total number of papers (f) documentation of ke~.,\"ordsfrom title published to the total number ofjournals in \\,hich the papers were published, and Publication The main concept of \\"orking on individual Concentration as the ratio in percentage of the scientist is to pr6\ride Ro/e Model Scienti.~t for journals containing half of the p"aperspublishedto ~.ounger generation of science graduates and post the total number ofjournals in \vhich thosepapeis graduates who ha\re. become frustrated due to were published during the period under study. \arious reasons. To sho\\" them light or hope or Sen and Gan [46] defined Producti\"it~. n~,\" direction to\\ards success. Success of others Coefficient as the ratio of 50 percentile age to the ma~' teach man~' things to folio\\. their path, The total productivit). age. attempt however small, ma~' prevent them to make Lawani [47] defined (Table -8) Synchronous suicide of their creati,ri~.- and channelise aggressive Self Citation rate : energies of~routll towards constructive ideas [ II ], A successful scientist is one who keeps on publishing his ideas or \\.orks. To be successful, Qpacit." to communicate effcctivel~. and cfficiently is most fundamental. Scicntific communications Frcquenc~" ofke~,vords from tIle titles of the ha\ "t: tlleir own rcgimc and rcgimcntatiol1 crossing articlcs \\.er~ rccorded. D~ta obtained from abo\'e all political and gcographical boundarics. stud~. \\"ere prcsented in tables and figur~s.

3. Methodology 4. Results and Discussion Scientific publiC.ltion, seemsto provide thc best During 1928 -1990 S. Chandrasekhar had available basis for measuring researchoutput. One published 380 research communications in the

JlSSI+2(2-3) June -September 1996 121 KADEMANI, KAL Y ANE AND KADEMANI following domail\s autl1orships in collaboioation with S. Clt'lJ1drnsekhar in Chronological order ofthcir association (in first publication with S. Chandrasekhar) are depicted in Figure I. Most active researchers and thcir contributions with S. Chandrasekhar were N. R. Lebovitz (22) and D. D. E1bert (15). Other activc collaborators with S. ('handrasekhar 'IJ1d thcir Gontributions wcre 13.C. Xanthopoulos ( I G). G. Munch (8), al1d F. H. 8reen (6). Otht::r collaborators having thrce papers each were 12, two papcrs each wcrc 20, and single paper cach wcrc 28. 8. C. Xanthopoulos had collaborated with S. Chandr[1.sckhar in the domain H onl~.. D. D. Elbert had collaborated with him in thc A. 8, E. F and G. whcreas N. R. Lebovitz had collaboratcd in thc domains E, F, G and H. Domainwisc Collaboration of S. Chandrnsckl1ar Table 1 shows author producti\rity and with his 47 Collaborators and their status of distribution of authors in ,.arious domains. -nlC autJlorship in various domains is provided in Tablc -2. research group of S. Ch.uldrasckhar has thc crcdits S. Chal1drasckhar had sillglc authored papcrs ill of numbl;:r of allthorships in \rarious domains : various domains as A(63), 8(34), C(39), D(2), A(91), B(~O). C(71). D( II ), E(43), F(42), G(~3), E(30), F(14), G(43), H(25) \lI1d (17). Hc had H(61). .Uld 1( 19). Total nllmbcr ofautllors in tllC collaboratiolls in various domains as A(2K), 8(40). rcsearch group wcrc 4H. Rcsearchers and tllcir C(32), D(9), E(13), F(2K), G(40), H(36) al1d 1(2).

Table Author Productn.ity nnd-Distribution of Authors in Vnrious Dllm.lins

No. of Dom;lillwisc AuthorshiDS No. or Total No. of Prominent

papers A' B c I-D, E-r-F rG AutJlors ~, Aulhorships Collaborators 8 I ~ 2 ~ 2H 2H

2 5 7 .f 4 10 20 3 6 " ~ 12 6 () Breen, Fo Ho 8 8 Munch, G. 10 10 )0 Xanthopouloso B. C. ~ 2 )5 Elbcrt,.D. D. 22 9 22 Lebovitz, N. Ro

55 36 2!< IX 380 Chandrasekllar, S.

Total 1.)1 ix() 43 42 JX~ I (iI 1\) .JX 501

:22 JISSI .2(2-3) June -Scptcmber 1996 SCIENTOMETRIC PORTRAIT OF NOBEL LAUREATES. CHANDRASEKHAR

s.o ~~HA-ASEKHAR M. R- L E ao"lTz

i 0. 0 ELBERT . ~ --- \ ~ , -- / - K O X - ~ C ~/ e.t XANTHOPOU'-°s .. O G. MU ~C...

K ~ - Z =- Z F. H. BREEN -

Q 0 QOO o C!JQ0 ~ Q Q 000 OG 0 0 e ~ eeo 00 CC. O G QOOQO Q 0 O G

OL ---t-"' I I ~ 5 10 ZO ~~ 'SQ ~~ .0 ...a ..8 - -R£SEA~CH£. S ~

Fig. 1. Researchers Association in Chronological Order

Percentagewise contribution of authorships to particular research field and once he felt that he various domains include A(18.l6), G(16.57), has exhausted everything in that particular field B(15.97), C(14.17), H(12.18), E(8.58), F(8.38), then he would summarise the whole worlc in the 1(3.791 arid D(2.20). fontl of an authoritative monograph andthen move He had published two papers in collaboration on to another field. v.ith the Nobel Laureate Enrico Fenni in the domain It is clearly visible from the Figure -2 that C during 1953. Chandrasekhar shifted his researchdomains very His domainwise cumulative number of frequently. That is how he continuedto remain very publications, his age, and scientific career active in the field. advancements are depicted in Figure -2. How does one not become an expert? A feature of Chandrasekhar's career was that Astrophysicist S. Chandrasekhar gave a he would \vrite a very long series of papers in a remarkable television interview a few years ago.

~

~ ~ c %

~

~v

Fig. 2. Domain\vise Publication Productivity .of S. Chandrasekbar Scientific Career AdvanernenL" .a = Govt. of India Scholar. Cambridgc: Univ .; b = Fellow, Trinity Collegt:. Cambridge Univ .; c = Res.Assoc. , Yerkc:s. Obsc:rvatory .Chicago; d = Asst. Prof.. Chicugo Univ .; e = Assoc. Prof.. Chicago Univ..; f = Prof.. Chicago Univ ..9 = Disting. Scrgice Prof. of Theoretical Astrophysics; h = Morton D. Hull Disting. Service Prof. of Theoretical Physics; i = Prof. Emeritus.

123 ~ nSSI .2(2-3) June -September 1996

~ KADEMANI, KAL y ANE AND KADEMANI

He had lead a Scientific Career notablc for a rate rescarch field more often than the less productive ofproductivit}' tJ1athas not slowed down at all into researchers [50]. his 70s. When ~ked how hl; has avo}dl;d thl; drop Howcver, no two individuals C:u1be identical in creativity m1d productivity that plagul;s mm1y in their creativ it)' i .e .each indi:vidual scientist has scientists, he replied tJl~t :lpproximatcly I;very scvcn his/her own Stereotype r51] and Mf!ntor [52-53]. years he takes up a new topic. He found that he Hence, attempts to generalise may fail. would run out of nl;\V idc:1S ~cr working ill m1 With timc :u1d adV:u1CCSin rcsearch a creative W'ea for too lung. 11lis p:1ttl,\m Icad him to l~ckll; sci~ntist builds-up his/hcrown rcsearch team. As such topics as tJ1~Jyl\.UlliI.:S of~l~llur sy~ll,\ms. whit\; pion~er has aI ready cstablished himselfhc becomes dwarfs, relativity aJ1dr~diative transtcr. Although pivote around whom entire team revolves in spirals all these subjects arl; in astrophysics, they arc (not in circle, because in circle there is no different enough to prcsent unique problem [48]. adv:u1cement as end meets the beginning) the With advances in research, vision of scientist direction and progressive movement ofth~ spiral expands. one island of superspecial isation or micro- shifts its prQgress slowly to next higher stratum theme expands aJ1dbridgl,\s connection with another every timc. Lcader or conductor of the orchestra island ofmicro-tht:me. A crcative researchertra,:els has the responsibility to bring forth best in evef)' through the bridges to othcr islMd aJ1d instcad of individual. Thus with advancing age many returning to his original island such scicntists individuals and groups join such an individual for continue to colonisc and work on the latest theme their own individual success as well as to satisf)' of fresh interest due to intrinsic motivations which affiliation needs. accelerote vigorous activities further aJ1d exploit Quinquennial publication productivity of new idea resources. Natives (Super Specialists) of S. Chandrasckhar is shown in Figure -3. Highest that island (micro-theme) may have become Collaboration coefficient was 0.5 during 1983-87 complacent because ofinbreeding of their thoughts. His productivity coefficient was 0.46 which is clear Creativity predominant in scientists is of two types: indication of his high publication productivity Convergent thinking creativit}' and Divergent behaviour during early period of 29 years of thinking creativity [49]. research publication career. The most productive researchers have changed His first paper was published in 1928 in Indian

Fig. J Quinquennial Public..tion Productivity of S. Chandrasekhar

124 JTSSI .2(2-3) June -September 1996 , -0""

SCIENTOMETRICPORTRAIT OF NOBEL LAUREA TE S. CHANDRASEKHAR

.Iournal (!f Ph)'.\"ic.\"at 18 ~.ears of his age in the in T3ble -.3 He has published 139 papers in The domain A. Astroph.~'sical Journal, 59 papers in Proceeding~. Distribution of his. 339 publications were in ~f the Ro.\'al .)ociety A, 3 I papers in Monthi.v 46 .i oumals, 16 chapters in books, 16 confe;rence No(ice.~ o.f the Royal A.~tronomical Socie1)'. 14 proceedings and nine books. papers in Proceeding.~ o.f the National Acad2m)' ]oumal".ise scattering of publications of of Sciences. He has published 10 papers in the S. Chandrasckhar in various journals is provided journal Observatory.

Table 3. Joumal\\ise Scattering of Publications of S. Chandrasekhar

I. Astrophys. J. 2. Proc. Roy. Soc. A. 3 Month. Notic. Ro~..

Astron. Soc. 31 9.1 67 .5 1931 198~ 54 2.579 O.~60 UK

4. Proc. Natl. Acad. Sci. 14 4.1 71 .6 19:?6 1963 8 10.480 1.~36 us. 5. Observatol!. 10 3.0 74 .6 1933 1972 40 0.814 0.227 UK

6. Philos. Mag. 9 2.7 77 .3 1930 1957 28 UK ., 7. Nature 2.1 79 .~ 1935 1990 56 22.139 5.224 UK

8. Phys. Re\,. 2.1 81 ..J 1949 1971 23 US 9. Proc. Camb. Phil. Soc. 6 1.8 83 .3 1935 1955 21 UK 10. Zeit. Astroph~.s. 6 1.8 85 .1 1931 1937 7 Gem.iI1y 11. R~,. Mod. Phys. 5 1.5 86 .6 1943 1949 7 14.071 1.759 US 12. Science ~ 1.2 87 .8 1944 1981 38 20.967 3.600 US 13. Am. J. Ph~.s, ~ 0.9 88 .7 1969 1972 4 0.563 0.134 US 14. Contemp. Ph~.s. 3 0.9 89 .6 1973 1980 8 1.541 0.111 US 15. Ann. Phys. 2 0.5 90 1 1957 1958 4 0.608 0.509 LTK 16. Mathematika 2 0.5 90. 6 195-+ 1957 4 0.69-\. 0.000 LlK 17. Philos. Trans. Ro~'. Soc.

London 0.5 91.1 19511 1952 3 182 0.237 LTK 18. Proc. Am. Philos. Soc. 0.5 91.6 1939 196~ 26 US. 19. Am. Math Monthly 0.3 91.9 1954 195~ O.19~ 0.111 1 US 2{). A1m. Ncw York Acad.

Sci. 0.3 92.2 1943 1943 0.830 O.I.JJ us 21. Astrofisika 0.3 92.5 1988 1988 Russia 22. Astron. J. So,.. Union 0.3 92.8 1934 193.. Russia 23. Astroph~.s. Nor\.egic 0.3 93.1 1964 19(H Nonv;ly 24 Bull. Am. Acad. Arts &

Sci. 0.3 93.~ ItJH9 198;9 us 25. Bull. Am. Math. Soc. 1 0.3 93.7 1947 19.J7 0.857 0.1-'7 us

continued.

~ JlSSI .2(2-3) June -September 1996 125 "' i KADEMANl, KAL Y ANE AND KADEMANI

26. Can. J. Phys. 0.3 94.0 1951 1951 0...1.61 0.099 Canada 27: Commun.Purc Appl. Matl1. 0.3 94 .3 1967 1967 1.080 0.167 us

28. CUrT. Sci. Q3 94 .6 1985 1985 0.253 0.075 India

29. Ind. J. Phys. 0.3 94 .9 1928 11)28 1 India

30. J. Astrophys. Astrol1. Q3 95 .2 198~ 1984 O.~64 0.105 India

31. J. Ind. Math. Soc. 0.:1 l)5 .5 IIJ60 1960 India

32. J. Math. AI"II. Appl. 0.3 l)5 .M IIJ60 1960 0.291 0.081 US

33. J. Matl1. Mcc1l. 0.3 9(j 1.1 1961 1961 US

34. J. Ration. Mcch. Amll. 0.3 9(j I.~ 195~ 1954 US 35. Mem.Soc.Roy.Soc.

deLiegc 0.] 96.7 1935 It)35 France 36. Nord. Astroll. Tidskr. 0.3 97.0 1935 1935 Norway

37. Notes. Record. Roy. Soc 0.3 '17.3 1976 1976 UK

38. Phys. Rev. Lett. 1 0.3 97.h 1965 1965 US

39. Physics Today 0.1 97.9 1971 1IJ71 US 40. Proc. Am. Acad. An. Sci. 0.3 l)X.2 1957 1.)57 us -4-1. Proc. Lol1d. !'vlau\. Soc. 0.3 ')K.5 195\) 1~59 O.64q O.18H UK 42. Pub. Astroll. Soc. Pacific. O.J 98.H IY52 1952 .047 0.006 FrdncC -4-3. QlIan. J. Mcc1l. Appl. Maul. 0.3 99 1955 IlJ55 0.567 0.115 UK 44. Quarl. J. Roy. Astrol1.

Soc. 0.3 1)9.4 1980 11)80 0.514 0.042 UK

45. Scientific Month. 0.3 1)9.7 19~7 1947 US

46. Truns. Am. Philos. Soc. 0.3 1 ()(I .(I 195~ 11)54 US,

TOlill 339

FPY = I:ir:;t Pupl:r Puhl ishing Y I:ur; LPY = Lust Pupl:r Puhl ishing Y 1:,lr u: = Impact l;'uctor; II = Immc:diuc:) Ind~x; IF ullc.lll vulul:s tukl:n li-um SCI Jour11ul Cituliullltl:port:l \')92-

In the highest lmp;lct Factor (22.139) journal Russia t\vo c;lCh, and C.Ul:1da.uld Gcnnany one each. Nature hc has publishcd scven papers. In other Avcragc Bradford multiplier was 3.46. highest Impact Factor (20.967) journal S'(..ien(.'(.'hc Publ icatiol1 dcnsity was 7.37 and Publication has publishcd four papcrs: I~eviews in Jvl()dern col1ccl1tr:ltion was 4.34. Phyj'ics having Impact Factor (14.017) whcrc hc 111Cfn.:qucncy and cumulative numbcr ofpapcrs has publishcd five papcrs. publ ishcd joLlmalwise is dc;:picted in Figure -4. Thejourn.:l!s trom vaJious countrics pllblishing Kcy\\'ords in thc titlcs of thc articlcs wcrc S. Chandr:lSckh:1r's n:sc:lrch p:1pcrs wer~ 21 from countcd. The data arc provided in Tables 4 and 5. USA (4565%), 13 from UK (2~.26%), tour from From thc data it is rcvealcd that thc titlcs \Vcrc India (8.70%), whcrcas from FraJlce, Nor\vay :lild vcr)' compact and expressive [54].

126 JISSI+2(2-3) Junc -Scptcmber 1996 SCIENTOr..1ETRIC PORTRAIT OF NOBEL LAUREA TE S. CHA.NDRASEKHAR

.P 3.0 ...,," o CUMULATIVE - - i3Z0 CJ FREQUENCY 100 ~ soo 100 $pS 1280 t 50 ~ 4 0 - z - ~ - 3 0 0 -' ~ Z 0 / - G ~ ... a.. " .c a.. 10

~ O Q / - ~ z ... .. ~ ~ -- 3 ~ :.60 - 2 0

I 2 3 ... s 10 4Oao .lOURNALS(LOG. N)-

Fig. 4. Bibliograpb on Papers of S. Cbandrasekhar

Table 4. Length of Article Titles in Tenus of Number of Ke~'WOrds in the Titles of Publications of S. Chandrasekhar

No of Ke\\\"ords No. ofpublications Percentage

ONE 52 13.69 4~ 68 l TWO 166

THREE 99 26.05

FOUR -1-() .0.51

FIVE 1(1 2.6:1

SIX 12 3.16

EIGHT 0.26

~ nSSI+2(2-3) June -September 1996 127 KADEMANI,KAL y ANE AND KADEMANI

Table 5. Domaimvise Keywords in the Titles of Research Papers of S. Chandrasekhar

Domain Total No. Total No. of Mean Per Title Proportion of Keywords

of Words Keywords No. of No. of to No. ofWords Words Keywords

A 623 166 8.09 2.16 3.75

B 470 115 8.55 2.09 4.09

C 513 140 9.33 2.55 3.66 " D 39 12 7.80 2.40 3.25

E ~12 110 11.44 3.06 3.75

F 2H3 HI 10.11 2.89 3.49

G 7H1 200 12.40 3.17 3.91

H ~59 112 10.67 2.60 4.10

I 102 28 5.67 1.56 J 3.64

J6X2 tJ64 K4.06 33.64

40') .1 1 JO7 I).H4 3.74

The Keywords- ti.~qul.:ltcies in the titl~s oftltc almo.\,phere (30). Equilibrium (26), Magnetic papers is provided in Tables 6 and 7. High fields ( 17), Stars ( 17). Gaseou~. mas~.es (9) and frequency Keywords werc .)tahility (39), General Kerr black hole (9). Relativity (35), Radiati\1(' I!quilihrillm (30). .)tellar

T.,blc (i. Kc)"vorll Frcquencic~ in the Titles of P.,pcrs by S. ('hlmllru~ldlur .

Stability 39 Colloidil1g wavcs 6 Generdl relativity 35 Dymlmical friction 6 Radiativc equilibrium 30 GrJvitutionul \\,uves 6 Stellar atmosphere 30 Hydrodyl1an1ics 6 Equilibrium 20 Intcrior of stars 6 lvlagnetic fields 17 lsotropicturblllencc 6 Stars 1"7 Oscillulions 6 'Gaseous masscs lJ Posl-Ncwlolliul1 crrccts 6 Kerr black hole lJ ThcmlUI il1Slubilily 6 Instability H Ul1ifom11y rotuting bodies 6 Perturbation theol)' H Absorpliol1 coemcicnt 5 Rotating c~'lindcrs H Axisymmetric perturbations Fluctuations 7 Brighuless Hydrodylulmic slability 7 Dcfonncd figurcs Negative hydrogen ion 7 Equutiol1s 5 Statistical theory 7 Gruvilul ionul perturbations 5 Stelar dynamics 7 Viscous flow .., Jucobi cllipsoids 5 Astronomy 6 A.'(isymmetric syslcms 6 continued

128 JISSI. 2(2-3) June -September 1996 SCIENTOMETRIC PORTRAIT OF NOBEL LAUREATES. CHANDRASEKHAR

Ma c Iaurin sphero ids 5 Stellar ~ 3 3 Milk.'" way 5 Stellar structure Non-l3dialoscillations 5 Super po tentials PoS1-Ne\\1onianapproximation 5 Tlffie reloLx3tion Reissoer -Nordstrom black hole 5 Uniform!.,' rotating configuration 3 Stellar ~'steIIlS 5 U~.erse TwbnlClce 5 Variab le-dCtSit)' 3 V trial theorem 5 Adiabatic invariants 2 Distorted pol)1ropes 4 A.'\iS}~c tmbulence 2 Fluid motions 4 13Canis M:ajoris stars 2 Gra\'ilational field 4 Caudty OOrlzon 1. Gra\'ilational radiation 4 Clusiers 2 Gravitational stabili~' 4 Coa-xial cyfinders 2 2 Hydromagnetics 4 Compton Scattcing Layer of fluid 4 Congrumt Dar'\\--jn~ids 2 Random disuibution 4 Conservation laws 2 Rotating gaseous masses 4 Dedeir.ind ellipsoids 2 Sla ti ol1aI".' . -t" Degeneration cores 2 Stellar configurations 4 Densit)' 2 2 Absorption 3 Differentially rotating configurations .. Absorption lines " Diffuse reflection 2 DistribtItinn 2 Astr()physics 3 2 Beau~' 3 ~'Jl3mical instability Black holes 3 D.'-nami:calStability 2 Coriolis 3 D~-narni:cs 2 Einstein 2 Decay 3 Eddington. A. S. 3 Evolution 2 E:\-pansi;Qnof functions 2 Ellipsoidal figures 3 Force -free magnetic field y E:\1endedstellar atmospheres Fourboundar)' conditions y Fluid sphere Incompressible fluid 3 ~orces Ionization 3 Functions Gn. m([1) ., '2 Kerr geometr)' Genefal variational principle .. Homogeneous mass 2 Magneto hydrodynamics -, 2 Miline. Edward Arthur Infinite homogeneous medium 2 Ne\\' statistics 3 Inhibition of convection lntcmal motions 2 Opacity 3 2 Planet~' nebulae ~ Invarianrtheo~' 2 Sch\varzschild black hole 3 Inviscid nO\\' Science Stellar coefficient 3 'continued. 129 JISSI+2(2-3) June -September 1996 KADEMANI, KAL y ANE AND KADEMANI

Ionized gas 2 Radiative transfer 2 Kerr metric 2 Rate of escape 2 Low density 2 Reflexion 2 Magnetic rotution 2 Reversing layers of stars 2 Motions 2 Riemarnl ellipsoids 2 Negati"e oxygen ion 2 Rotating configurations 2 Neutrino waves 2 Rotatulg fluid sphere 2 Newtonian gravitation 2 Roche ellipsoids 2 Oort. J. H. 2 Schwarzschild limit Oxygen 2 Slow rotation Polarization 2 Solar chromosphere 2 Post-Newtonian cquations 2 Sunlit sky 2 Pressure 2 Thermodyllamics 2 Pulsation 2 ; Transmissioll 2 Pursuit of scicnce 2 'Viscous dissipation 2 Radial accelcrat ion 2 White d\\';}rfs 2

Table 7. Key\vords Used Only Once in the TitleN of Papers by S. Chandrasekhar

Absorbillg atoms Blmtkcting crrcct Constitution or St(lfS Distortcd polytropcs Absorption COnIinllum Blcndedabsorption lines Continuous spectrum Distorted stellar Adjoining mcdia Bowldary value problcm Convection configurations Ad.loint dlffcrcnt ial Bro\vnum motion Coriolis (Icceler'.ltion Double pcriods system!; Cartcr's tllcorcm Coronll Double -star problem AeastJletics Central R:ldiation COrrel(ltioll Einsteill's field cquatiolls Anlplifications pressurc Cosmic magnetic fields Einstein Maxwell Angular distribllt ion equations Centn1l1cmperature Cosmological constants Arbitrary spill Einstein -Maxwell space CcIltrJlly condcnsed Cowlirg's theorem times Astrophysical colldition!; st,lrs Cur\'ed cll(1!1ncl Astrophysical inlcrest Einstoin -Maxwell tlleory Ccntrifugal rorce Cylilldricul impulsive Einstein -Vacuum space Astrophysicist Charactcristic \'aluc w(lves times AtonlS problems Cylindrical \\'(1\'es Axisymnletric Electromagnetic Charged particles Dar\\'in ellipsoids gravitational fields . perturbations Chromosphere Asymmetric Degenerate cores Electron Collapsed configurntion homogeneous dyrulmos Density distribution Electron pairs Collision . A~isymmetric milgnctic Dirac, P. A. Mo Elements ncJds Compton crrect Dirac. equation Ellipticity Axisymmetric motions Condensation or stars Energies Beo1ts Configufiltions Oimcosviews Eridani B. Bell- Szekers spilce time Connectivc instability Dispersion Binary S)'stem Constants Dissociation fomlula continued. 130 JISSI .2(2-3) June -September 1996 SCIENTOMETRIC PORTRAIT OF NOBEL LAUREATE S. CHANDRASEKHAR

Evolution of stars In t egrd1 theDrern Odd -parity mode Radialtemperature Extended photo~heres Interface One-ifunpnsional gradient

Fmite distance Invariant theoI}. potemial barri ers Radiation Fluid conductor Ionization fmmula Onset of com-ection Rajagopal. C. T .

Flux integral Isothermal cores ()petation Rayleigh scattering Fourier -Bessel-type Isothernlal fimction Onbogonal functions Recombination Onostrnve Refle.-cionroefficients expansions Isotopes Outer layers Relatn-e abundances Fowler, Ralph HoVIard Isotropic scatt-ering FreqUClcy Jacobi sequences Pencil I3diarioo Relamistic degeneracy. Relati\'istic equilibrium Galactic evidences Jeans.janqes hopwood Perception ofbeaut)' Gaseousstar J eans s~ Perfectfluid Relativistc instability l ~ Jeans sp~ PernubariOD analysis Relativistic statistics ! Geodesics Photographs Relativistic systems Gode1'sUniverse L4n1e -Emsdo:t function PhysiQI content . e 325 Relamistic theory Ground states of Helium Limiting Clse Physica.l st31eof matter Ground states of Rid11myer Lithium ions Limiting mass pbysicaI theory Rochemodel Ground states of oxygen L in ear pernIrl:rat:ions Physia Roots of ions Lindbald- s theory Pin riyer i -(I + Y:) (An)II+ If: (I..) Hartree field Liquids Pinch 11+ I/,. (i.n) i - Heavy viscous fluid Maclaurin sequences Plane grdvitational (i.+ 1f2)N = O Heisenberg's elementary Magnetic ~ Plane -parallel Roots of theo~' stars annosphere High order differenial Plasma. Yn(l..n) 1n(A) -1n(An) Mass 1ess paniI: 1es Yn(i.) = O equations Plasma physics ~ Maxwell's equations i' High ~eed atoms Rotating liquid drops ~ Post -Galilean Metric pertw;bations Higher order virial trnnsformati on Rotating stars Motions 01 dlarged equations 211:zPost -N~1onian Rotational distortion panicles " Highly collapsed equation Rotational problem f configurations Motivatioos Po-51 Newtonian Rotational velocities Historical account Moving ;l1,.",~Jhere methods Rotational masses Homogeneous Post-Ne\\1OniantheoI")' of compressible model Multiple frequencies Rotating pol~1ropes Einstein Nebular l1IminDsit)" Royal Astrono.mical Homogeneous ellipsoids Potential barriers Socie1.'. Homogeneous turbulent Nebulliurnemission Potentials Rumford Medel Lecture medium Newtonia:n-tl1eory 1957 Probabilit." distribution Horizones Non-axisyrnmetric mode Russel. H. N. of oscillation Probability method Human culture Scattering of ra,diation Non-dissipative couette Prominences Hydrogen atom Schwarzchild geometrics flo\v Quasi nonnal modes Hydromagnetic Scientific allitude oscillations Nol1-stational)' penurbed Radial ejection systems Scientist Radial oscillation H)'Perbolic equations Novae illumination Null dust Radial speed continued... Integral equation Nutku-Halil solution Radiation reaction

nSSl+2(2-3) June -September 1996 131 KADEMANI, KAL y ANE AND KADEMANI

Teukolsky's equation . Second hannonic Stationary perturbed fields oscillations systems Teukolsky -Starbinsky Unifonn rotation Second post -Newtonian Statistical basis constant Unifl?nnly rotating fluid equations Statistical turbulence T1lennal convcction masscs Secular stability Stellar absorption lines T1lcoretical astrophysics Vacuum mctrics Semi -infinite Stellar encountcrs T1leof)' of relativity Variable viscosity Variational methods 3tmosphcres Stell3r envelops T11ird hamlonics Sequencc Stellar evolution Tidal distortion Velocity ellipsoid SimulU1cous action .Victor ambarstsumian Stellar models Tidal problem Singularities Virial equations Stellar photosphcres Timc -scale SmaI1, W. M. Virial relations Stellar Scintillation Timc -like sinb'Ularitics Softening of radiation Viscid flow Stellar statistics Total cclipse of the Solar research Viscosity Stochastic problems Solar system origin Transfer of radiation .Viscous liquid globe Stocl\astic variation Source of energy Tnulsfom1ation W eizsacker theory Strings Transmission Spatial correlations Weyl'ssolution Sun coefficients Speed of fluctuations Ii S State of helium Trumplcr's stars Spherical shells configtlration Trutll and beauty Spirdl amls Tempcrdtures White dwarf stars Tensor virial equations Spiral no\\' T",o black holes Wolf- Rayet stars Star- Streaming of high rmtk Two centre problcm X -functions State or mattcr Terrestrial conditions Two commuting killing y -functions

These key\\'ords indicate his wide spcctrum of to undcrstand them very easily. One is awed by thc interest, matcrials, mcthods, instruments llscd and depth of his physical acumen the range of his subjects addrcsscd to in thc collrsc of his 63 )fears mathematical vision and the sweep of his t)frcsearch papcr publishing lifc Sp:lJl, 3Stronomical knowlcdge. He W3S a confluence of Domainwis~ bibliographic charoctl.'ristics of Mathematician, Physicist and Astronomer in publications of S. Chandr.1sckhar are providcd in himself. Tables 8 and 9 Highest number of equations pcr paper werc It is cvidl:nt from thc publications of S. 127.4 in the domain D. 108.3 in thc domain B, and Chandrasckhar that th~). are full of Mathl:matical 107.4 in the domain H. eqllations. It is \,1:~. difliclllt tor an ordin:lf)' rcadcr

Tahlc H. Domaim\'i!lc Blbllographical Churactcri!itic!i per Puhlication of S. Chandrasekhar

132 JISSI .2(2-3) June -September 19~)6 SCIENTOrvlETRIC PORTRAlTOFNOBEL LAUREATE S. CHANDRASEKHAR

,~ Table 9. No. of Pages per P.lblic-- of ho,,- his career would have unfolded had he S. Chand rasekbar remainedin lndia- Like Raman,his uncle, he might have presided over his oWn institute, but he then \\-ould have becomeenmeshed in the oIC3llepolitics oflndia-s scientific establishment [9]-

5. Conclusion S. Chandrasekharhad contributed 380 papers during the period under study to various domains : .)tellar stnlcture and Stellar atmospheres (77); Radiative tran.s:ferand negative ion ~f hydrogen (55): St'Jchastic, Statistical hydrodynamic problems in physics and astronomy (55); Plasma ph)l'Sic.s(5); H.vdN}magnetic and hydrodynamic stabilit.v (36); Tensor -Virial theorem (28); Relativistic Astrophysic.s (63): Mathematical theory' of Black holes and Colloiding Waves(43): Ntn1T,bersof figures per paper \vere three in and General ( 18). . the domain H and ~.o in the domain B . He had 267 single autl\orship papers, 105 two Num-ber of tables per paper were 2.7 in the authorship papers, and eight three authorship domain F, 2. I in the domain A, 1.9 in the domain papers to his credit. E, and 1.5 in~ domain B. His 47 collaborators have contributed 421 Self citations per paper \vere 4 -9 in the domain authorships and domainwise collaborative F, 4. 0 in the domain H, 3.9 in the domain G a.'1d authorships \\'ere A (28), B (46), C (32), D (9), 2.0 in the domain C. E ( 13), F (28), G (40), H (36), and I (2), Citations to other authors per paper \vere 8.8 He has published 139 papersin Astrophysical in the domain C. i.6 in the domain B, 7.1 in the Jouma1,59 papersin Proceeding,sof Royal Socief)'- domain H, and 6.3 in the domain A. A. 31 papers in Monthly Notices o.f Ro.\'aJ fl S~"Dchrosous self citation late forthe domains Astronomical Society, 14 papers in Proceeding.)' \vere A (11.1+), B (20.23). C (18.46), D (12.12). o,f the National Academy of Sciences. and E (40.57). F (50.00). G (43.02), and H (36.32). to papers in Ob.)'ervator;'. Mean S~.nchronous self citation rate \"\'35 24.44 High frequency keywords in the title of his \vhereas meanS\,-nchronous setfcitarion rates \vere papcrswere. Stabilit}. (39); General relati\it}. (35); for C. V Ram:in (15.05) [29] and for Radiative equilibrium (30): Stellar atmosphere K. S. KrishD3D i 13.82) [33]. This has sociological (30): Equilibrium (30): M~netic fields (17); Stars implications Indicating that S. Chandrasekharwas (17). a highl~. productive and ke~. figure in his research Mean bibliographic characteristics ranged : specialit.'. [47}. .Equations (47-127): Figures (1-3); Tables.(1-3): NumbeT of pagcs p~r publication of Self Citations (1-5); Citations to others (5-9): S. Chandrasek:irar are provided in Table 9. S~.nchronous Self Citation rate (11-50); Pages (11- India inspite ofits timitations has produced so 20). man~' illustrious scicntists like H. J. Bhabha. J. C . Considering all above bibliometric indicators, Bose. C. V. Ram:lO. S. Ramanu.jan, M. N. Saha he represcnted ex~llence in his performance and :lOd can producc so mJl1~. scicntists ofhigh calibrc had set up vet:. high standards for his follo\\'ers to provided it pro\.ides congcnial scientific climate surpass it. His work. can be considered as for scicntists to \vork. perfom1anc:e of a Role Modcl Scientist t

133 JISSI .2(2-3) June -September 1996 KADEMANl, KAL y ANE AND KADEMANl

References

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