Criteria for the Discovery of Beta Cephei Stars According to the Mu -Mechanism Theory

University of Nebraska - Lincoln DigitalCommons@University of Nebraska - Lincoln

Norman R. Simon Papers Research Papers in Physics and Astronomy

6-1970

CRITERIA FOR THE DISCOVERY OF BETA CEPHEI STARS ACCORDING TO THE MU -MECHANISM THEORY

Richard Stothers Goddard Institute for Space Studies

Norman R. Simon University of Nebraska - Lincoln, [email protected]

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Stothers, Richard and Simon, Norman R., "CRITERIA FOR THE DISCOVERY OF BETA CEPHEI STARS ACCORDING TO THE MU -MECHANISM THEORY" (1970). Norman R. Simon Papers. 55. https://digitalcommons.unl.edu/physicssimon/55

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© Publications helium of has temperature), Astronomical character. and new following original total evolve primalY reaches secondalY, velope tions binaries we burning valiations radial raise in Percy CRITERIA Hill Leung. In f3 Recent favor Obselvational occasionally refer been f3 Cephei (1967), a mass of the Cep and of (1970). pulsations by first, with recent the its the Additional primalY of reactions the compiled and A lists effective stars. nitrogen Astronomical theolY the RICHARD Society in stars exceeds this Roche which list primalY's spectral narrow reader expanding Leung then, light positively weight FOR of Earlier paper STARS The of discriminants as theolY Goddard MU of the star, potential of for overabundances, which advanced in Society lobe. accretes the data for temperature and (occasionally on 6 type numbers f3 STOTHERS THE -MECHANISM (1967), "classical" the the Pacific of (Stothers WC core. being lists support, details can Cephei Receiv.ed top of thus its ACCORDING radial the o 09-B4 Thereupon the core. benefit NASA, are Institute , f3 I. by be Pacific, radius are the DISCOVERY of first are far • helium Cep McNamara If more Introduction Provided strongly not of the Stothers found that, accumulated III velocity, sufficient Considerable referenced, proposed stars. .'tafch f3 compression broad) and Vol. AND of 707 the New and candidates, far f1-mechanism suspected -V Cep covered during for 82, massive observers (}L ultraviolet the outer and it Simon by in No. NORMAN 19, to York and Space mechanism) In stars, spectral will energized the 487 our THEORY to helium-enriched pelmit 1970 can and a helium a hydrogen Simon TO (June are in NASA test large zero-age comprising for than close qUickly original f3 interested with OF 1969) Studies the theory. of be flux observational not Matthews 1970), line Cep the THE example, R. Astrophysics orbital the (1969). the found following. BETA is the excesses confilmed in binalY by SIMON p. pp. has we widths, accreted -mechanism contradiction stars lose secondary's envelope burning paper, development 707-715 secondalY, 24 in the been ratio proposed These in searching by spectroscopic mass (high (1967), CEPHEI system have outer hydrogen and papers Data of evidence to found Hill periodic and include: until masses, surface which of to binary theory System been with, por will and and en the the the the the for by to of it 1970PASP...82..707S © Percy 708 tabulated Cep group theolY, not ultraviolet 0-B3 these mass confinned. we we (3) cult abundance richment chemically as discovered and luminosity helium assumption is in 'Y Astronomical to how are 1959), classical and Mv The In correct, Detailed Pegasi O\lr low other shalp note = - = sufficient overestimated to now (6) other stars the much which ratio; II-V; models with (1970), expected as both detect we abundance, refer 4.5 that f3 early interest (or is Y and or considered and as flux Society slowly Cep for list of sufficient = the -too abundance unmixed 'we helium of (Stothers (2) (5) of referred broad) these (1) conditions for observationally but specifically, 0.6 8 helium 'II. slow, this chemically ,which B e~cess. the shall short-peliod particular helium stars, Ceti helium of the bright apparent stars. of (159)(0) rotating Helium the the pelmits most (deliberately) limits (se.e STOTHERS has interior spectral now uncovering fainter to'by {Neven to Il?odels, Pacific by and like'Y to seem properties' Individually, analyses destabilize overabundance However, to diffused Underhill and for basic consider mass be on aim ~nd and Petrie mixed " explain albeit B a Simon MK f3 • mixing f3 to variations Peg lines; moderately Y nitrogen Provided stars extremely and Cep because Cep and Nitrogen of observable Y at may show spectral AND are additional and = below and not further of models the the de stars in most 1970) such (4) 19(6). seem our stars. because 0.5 has actually these these' by available detail. "nolmal" Pearce Jager uniquely, 8 sUlface binalY SIMON only pulsational overabundance; the models. (309)(0). in (as Cet, of to in Abundances analyses the unreliable low to type that testing must Since light NASA Moreover, criteria properties the be is our suspects little show 1954; members we photosphere, (1962); actually are be sUlface character of adopted f3 and the for theory helium Astrophysics be and to criteria Thus, Cep lower ,Our have the velY surface In for.O -noticeable Aller are two damping revised faintest, our luminosity Hill this, have concerning, radial helium ,stars. validity models it observed). of necessary of slow may the subsequently still, if f3 with theory, with is and and and (3), connection, potential (1967), helium the our Cep yet Data fractional uncertain since Thus velocity; to be rotators, possible because 4, (5), (4), content Jugaku respect a B can helium f3 (6) in theolY of about to System large stars, diffi class stars Cep it and our but our the en the the far be be is f3 1970PASP...82..707S © mal" deficiencies· model trinsically present. are actually tive the of large though sociated with Astronomical only spectlum helium models fact ing B1 stars o B~sco,mbe extinction currently sidered sible) possibly Bles,s, for effective The We High In f3 V. to essential a effective secondary of that Cep with temperature addition helium star ,ten scatter values also early In Code, presence atmospheres, star the these , over meaningful. with relevant absolute This represent temperature measured any the stars ,in of slow difficulty percent Society which (1965), predict (Hardorp HD.96446, to ultraviolet effective temperature B around. the has and abundance measured early event, of "nonna}':> temperatures to verify DISCOVERY are products rotation (Byram, of of log chemical example yet at right becomes in Houck photometric the expected, error large B wavelength an sharp becaus~ III. the is very 'a to this IV. Furthennore" g stars, Pacific of those temperature and unquestionably overabundance. to different = be 10,000° direction continuum, expected 30,000° ultraviolet or Far in of point. Chubb, Spectral N/C scale high which .4.3-4.5 spectral, be of 1968; verified. composition the Strittrrlatter a • large the for old are this, Ultraviolet of on OF Provided of small and for helium temperatures, range the K. K nonvariables observed accuracy, hotter type our hydrogen Stecher examination, f3 is Underhill ultraviolet in Line hot and and (see 40,000° lines CEPHEI N/O models color relatively Stecher angle observed theolY, by and the A 0 stars overabundance the required Width Werner 1115-A than Te Bolun-Vitense anomalies, 1968). Fluxes ratios with in Good 19(9) far indices the NASA ultraviolet of = .... K burning coupled, a (1966) of points STARS to excess the implies 40,000-50,000° inclination the ultraviolet. star a small of finds in 3000 selective f3 at Therefore, be Astrophysics model should, shell 1965; to _ spectral ones deep f3 Cep for the finds ,may characterized the of obtain will out Cep it changes should an with known spectrum, flux sUlface, our may to line normally 1967). Smith stars atmospheres atmospheres not the.classical indiG~te be error that of interstellar be stars Thus, Data 40,000° the type at a detected alter detailed blanket the be also K of f3 defini of in a A in .. System "nor 1967; since As (pos 2000 may con type Cep line flux 709 late but the the the Al th,e in~ as by be K a .. 1970PASP...82..707S © of measured frequent their All substantiated radial-velocity spectroscopic possibly 710 f3 scopic known this sibility nOlmal bership (1969), (high radial basis 1967). should Astronomical component hard helium scopic binalY larly have B tions reliability II-V the Broad No At sight spectroscopic Cep of phenomenon, Orbi~l spectral in for to will, of the been rotation). searches the "beat" velocity, be. spectroscopic binaries who stars systems, to broad in to has light, detect. the all suspicion spectral the known present the rotational of a Society of become chosen is members Elements binalY width been discovered more course, period, according binary the the and so nOlmally axis lines CUlves for which binaries, with Instead, A of f3 that, bllt lines, available may fact time, f3 massive the suggested luminosity of that number Cep of pulsationally according system. STOTHERS of Cep depend which, and systems velocities rotation. Pacific the large of spectral of of even may B that be of members the they to we that we binary Spectroscopic listed a eclipsing giants stars evolved course, due star our number of • v. brighter if For mass be mass in some are have heavily are Provided the (e.g., independently the classifications, suspected to the lines, have Binaries All simply in (the due theolY. show example, systems. as AND reduced all unstable, the of brighter Batten's ratio ratios concentrated secondalY are are case binalY of and Batten well potential of binaries to intrinsically been on member by and criteria: the not SIMON to the abnolmally these the orbital of as Binary the One less f3 and as orbital Analysis classical it a a evelY to NASA carried incompatible (1967) potential 1967; brighter component Cep its (occasionally Vir Virginis long-period is exhibit has variables using massive f3 which by spectral and thinks spectral pulsations now motion Systems. Astrophysics Cep exhibits f3 on stars ~otion. Fitch accreted Sixth slow Shobbrook Cep out fluctuates f3 of the shalp known clear components a has is candidate) Cep candidates of also the long solely (Wolf-Rayet) types, a star rotators (e.g., Catalogue has, of other 1967, type Wolf-Rayet broad f3 with changes led Our uncertain) stars that would light This Data the show lines Cep sufficient showing spectro spectro in Breger irregu 09-B4 on to 0 1969). which et mem selec System well none with lines fact, star. pos and and and and the the the for for al. be of in of 1970PASP...82..707S © 9)( which nitudes chek, (1967). masses, er fainter Batten sec), Kopylov Yoss only that the systems earlier helium Astronomical luminosity the into brighter this ~ curves an with smaller detection than (Eggen Columns Columns Columns Columns 1 Columns Column The and 10 sin: remainder analogously star class connection, stars (1965), of likely the Conde, its WI are 3 (1967), available fainter of components, corrected in i MK overabundance, the except mass with and o star (1964), > > spectra] spectral A, .) eclipsing, with of parentheses) the Society 11: 1 5 3 class) (3 9 7 brighter or B, spectral In is not and and and Greenstein and 9)(2 smaller or is and and Cep most much of components Hill our DISCOVERY or that a class-C Slettebak Olson uncertain, only that of data narrow 2: mass the 6: for C. sin''3 4: than type. de type the 8: 10: classification (1967). candidates with spectral 9)( HD apparent anomalous larger orbital and from stars, Sierra type. all f3 Pacific 9)( mass i. indicate I as apparent (1968). and of its < systems, Cep Could as number Table sin: the of 1965). range fainter low (1956, its 109)(0. companion, by (or Batten suggested (MK is the orbital Class-B but 3 inclination, • (1964), type following variability i OF companion. Provided visual clearly analogy as smaller) (in I that, the are "helium systems is of 1963, Accurate and of f3 lists rotational classes 69)(0 the components, and solar CEPHEI probably period (Our (1967) Sahade B the color stars magnitude systems in name. by spectral the more luminosity above? spectral 1966, data. with than can the n some or system. are but theoretical when in units) white with selected Class-D in index NASA or else light (1962), shown our be velocity, evolved a that 1968), also STARS days, the are cases, Sahade Vir type It from available), destabilized, type masses of has Astrophysics (photographic dwalfs list In nOlmally and is the class same and similar which systems, underlined. the both systems Koch, Slettebak worth class-A of models may the the Boyarchuk be (has small v radial-velocity of spectral (1962). the brighter sin greater as are from an mass same does the Olson, pelmit a to associ

© --l 1J).> 1--1 ~ f.\O 101 0 TABLE I =0 :3..... EARLy-TYPE SPECTROSCOPIC BINARIES WITH A LARGE MASS RATIO ~ ~ -rJl 0 :)), 1 3 :))'2 3 VI ~..... HD Nrime In P SPI SP2 sin i sin i sin i V2 sin i Class ~ ~ (days) (:))'0) (:)J,0) (km/see) (km/see) ~ 0 ~ ~ B3 10.9 33 3369 29'iT And 4.4 143.6 B5V 26.9 A r:J). ~=- DO 10516 cP Per 4.1 126.6 B2 Ve 15 7.5 450 ~ "'= ~ 19820 CC Cas (7.0-7.1) 3.4 09 IV 09 IV 18.9 9.2 A ~..... 0 DO -~ 23180 38 _0 Per 3.8 4.4 B1.5 IV -III B2 V 5.2 3.6 75: 150: ~=* 25204 35 A Tau 3.4-3.9 4.0 B3V A4IV 6.1 1.6 117 Bo :t • ~ 94 T B3V 3.0 0.9 150 100 D 29763 Tau 4.3 3.0 AIV =:0 101"'= 0 33357 SX Aur (8.4-9.2) 1.2 B3V B3V 11.2 -5.9 A r:J). -<..... BO Co Q. 35715 30 t/J Ori 4.6 2,5 B2IV 8.7 5.3 166 > ~ Q. 37043 44 tOri 2.8 29.1 09 III B3p 15.9 9.4 100 50 D Z C" 37756 4.9 27.2 B3 III Bl 6.4 4.1 .87 Co U ~ r:J). ~ 39698 57 Ori 5.9 7.8 B2V B5 10.3 3.9 140 D ~ ~=- 42933 8 Pic 4.7-4.9 1.7 BO.5 III BO.5-3 16.3 7.3 270 Do ~ Z 65818 V Pup 4.1-4.7 1.5 BIV B3IV 18 10 180 A 0 >rJl > 104337 5.3 3.0 B1.5 V 8.2 4.4 143 D Z 116658 67 a Vir 1.0-1.1 4.0 B2V B3 V §l Q 172 DO 1J).> ~ 121263 , Cen 2.5 8.0 Bl-2 IV 6.4 4.4 200 D 101 0 ~ 144217 8 f3 Seo 2.6 6.8 BO.5V B2V 16.0 9.6 85 85 D ~=- 151890 p.I Seo 3.0-3 ..3 1.4 B1.5 V B6 14 9 220 D 1J)...... ~ 156633 68 u Her (4.5-5.2) 2.1 B3 III B5 8.6 1·3 119 90 D 1J). B3V A2 12.1 4.7 0 173787 V356 Sgr (7.0-8.0) 8.9 II A ~ 181987 Z Vu} 8.0-9.0 2.5 B4 V A2-3 III 5.4 2.3 B ~ ·53 Do rJl 187879 V380 Cyg 5.5-5.6 12.4 Bl III B3V 14·1 8.0 ~ 1J). ~ ~ :3 1970PASP...82..707S

1J).> TABLE I (Continued) ~ o101 =o :3..... -HD Name In P ~)Jllsin''3 i ~ll;2 sin''3~ i v 1 sin i v2 sin i Class ~ SPI SP2 u ~ ('))' ) ~ (d_ays) --'0 (~ll;0) (km/sec (km/sec) (J) -rJl o .- n ~..... ~ +40°4220 V729 eyg (10.0-10.3) 6.6 09 07f 7.8 1.9 C o ~ 208095 5.5 17,.3 B7 B9 20.8 1.3.6 A < o tr1 ~ 209481 14 Cep 5.6 .3.1 09V 09 5.8, 2.9 C ~ ~ ~ 214240 6.3 10.9 B3V B5 6:0 .3.9 60 D ~ 217312 7.4 15.3 BOIV BOIV 27.0 12.7 70 A ~"'= o ~ ~ 5 ~ ~ • ON6tes to Table I n tr1 "'= HD 10516: possihly variable in light with a short period (Lynds 1959)., - 101 ~ o HD 23180~varl~lble in light with- a short period according to Walker (1962), but probably constant ac<..:ording to Lynds -< ~ Q: (19~~).Jones (1960) found variability in the radial-velocity carve. tl:j ~ Q. 'HD 25204: a close triple system. _ . ~ C" -HD 35715: possibly variable in light with a short period according to Lynds (1959) and Hill (1967), the latter of whom (J) ~ ~ ~ called'the star tentatively a f3Cephei star. - ~ > HD_ 37756: variable in light with a short period according to Lynds (1959), but constant according to Hill (1967). ~ Z (J) HD 42933: variable in light with a short period according to Cousins (1966). ~ >rJl > HD 116658: f3Cephei light curve (Shobbrook et al. 1969)...... HD 187879: constant in light according to Hill (1967). 1J).> ~ HD 217312: constant in light according to Hill (1967). o101 ~ ~=- 1J)...... ~ --l 1J). I--i o c.v ~ ~ rJl ~ 1J). ~ ~ :3 1970PASP...82..707S © helium. their stars. and our And masses systems companion, we versations the Cep accretes writer changed Aller, Astronomical ably Finally, tration. - Jaschek, Associateship Cousins, Jones, B6hm-Vitense, Batten, Bless, 714 Breger, Fitch, Boyarchuk, Eggen, Koch, Byram, Buscombe, Hill, Hardorp, Leung, Our One b list 1969, secondalY G. HD behavior. e.g., some consist L. R. R. masses) W. D. A O. A. K.-C. list M. (N.R.S.) of E. 1967, because H., C., A. C., H., may H. J., we with S. few 208095. J., H. sufficient mass U us W. Ap. T., J. 1967, systems A. Code, by and and P. Olson, Society Conde, leading 1967, and should Cep, 1967, 1967, of 1966, (R.S.) may E. other Ap. Chubb, 1965, T. A., 1960, have no components Jugaku, of Strittmatter, under nonnal Greenstein, 158,269. (our in acknowledges L'l.N.R.A.S. 1967, A. of J. E. Ap. and of means stars , Pub. In Ap. H., L'I.N.R.A.S. be Sllppl. D., with any thanks their the L'l.N.R.A.S. binaries C." helium, Al.N.R.A.S. caution Phoenicis, to previously STOTHERS J. T. proposal fact, J. Kopyloy, J. the and and Ap. Pacific even DOlTl,illiOIl and 148, pairs the which 150, A., 1959, system a very 14, exhausts J. J. P. Sierra, Houck, National Yoss, small 136, Drs. the 48l. and 150, having 223. L. preparation 263. A. that more it in • 131,443. REFERENCES of 129, Ap. 120, large I. Provided 5l. 1965, last for have 1968, f3 would K. Werner, the the main-sequence K.-C. 483. Astrophys. A. which T. mass suffered most M. J. Persei, M. AND l. 43. the likely the E. C. support Supple two spectral Aeronautics nearly 9Jl 1964, Ap. Ap. accreted 1965, Leung de 1968, by function, of 1 possible not already • M. J. has SIMON J. stars the the 1964, of U It 4, ()bs. 141,83. lzv. candidates extensive 153,465. W. Ap. be equal NASA 109. is Ap. Sagittae, of this range suffered systems and have 13, also Crilneall J. 1965, La expected a J. an stars, candidates but known 141,955. and NAS-NRC 119. Astrophysics paper. 153, N. Plata spectral possible overabundance B5- been AIlIl. an J. mass 56l. in 1T Space and mass for Ap. Woolf Sere B9 invisible f3 Andromedae, class d'Ap. to The included that, having Cep have ()bs. Astr. types exchange. for that Data exchangt: exhibit Adminis Research D for 28, second f3 unless 31, stars). 28 prob System large some (hot) Cep con and 594. ex (2). 44. in of f3 1970PASP...82..707S © - - - - Lynds, Olson, Percy, Petrie, Shobbrook, Sahade, Neven, McNamara, Smith, Slettebak, Stecher, Stothers, Walker, Underhill, Astronomical Hack, Obselvatorio Publishing 1969, 1966, 1963, 1970, 1968, J. E. A. c. R. L., J. M. T. ed. R. L'I.N.R.A.S. R., C. R. A. 1967, M., and A. P. 1962, Ap. Ap. Ap. Ap. F. (Paris: 1970, R. and D. Society 1968, Co.). 1959, 1956, B. 1969, and de J. J. J. J. 1952, Astronomico, R., H., Simon, Ap. 151, 145, 138, 160 1966, in DISCOVERY Jager, C. Ap. Gauthier-Vilhu's), Ap. Pearce, Ap. of Herbison-Evans, Ap. and J. Synlposilllll 145, A.J. A.J. (in the 118. 126. 1043. J. 147, J. J. T. N. The press). 159, 74,98. Matthews, 13l. Pacific 153, 57, 130, 124, R. J. 1954, 158. Universidad Early 227. 177. A. 187. 1969, 577. 173. 011 • 1962, B.A.N. OF Provided Type Stellar p. G. Ap. D., {3 127. Plih. E. ].157,673. CEPHEI 12, Nacional Stars Johnston, Evoilitioll, by I 1967, 103. Donlillioll the (Dordrecht, NASA in de STARS I. .'Ioderll La J. Astrophysics D., Astrophys. Sahade, Plata), Holland: and A.~·t/'()I)hysi('s, p. ed. Lomb, 185. ()iJs. Data (La D. Reidel System N. 12, Plata: 715 M. R. l.