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General Disclaimer One Or More of the Following Statements May Affect General Disclaimer One or more of the Following Statements may affect this Document This document has been reproduced from the best copy furnished by the organizational source. It is being released in the interest of making available as much information as possible. This document may contain data, which exceeds the sheet parameters. It was furnished in this condition by the organizational source and is the best copy available. This document may contain tone-on-tone or color graphs, charts and/or pictures, which have been reproduced in black and white. This document is paginated as submitted by the original source. Portions of this document are not fully legible due to the historical nature of some of the material. However, it is the best reproduction available from the original submission. Produced by the NASA Center for Aerospace Information (CASI) i k f., _ ^ ^ _ ^y^ ^^ .^ ^ ^^ ^ ^. i ..,. ^^'^;^^^ Z rn ^ ^ ;(NASA — Ck-1+J$4$6J ^ONTFcIbUTFONS OF TfiE N76--G94$5 Q3SERVA3'QRX OF NE4i MEXICO 5 ?'iiTE JivIYETtSITY, THRU YOLC^Mr 1 , NQ. ^s, HnRII. 4 {Neu I;exico State N76 - 29695 L.^iv.) $4 ^ ^iC $5.00 CSCI. G3A ZJncias X3189 ^i6 U^i7 ^C3^tT'R^Q^1T^C?1^IS ^F ^^^ ^^^^^^^T^^^ ".aF h1E'Vof 1V^EXICC) STATE ^11^1iV'ERSlT`^ LAS CR^i^ES, I^EO/V NIEX^C;® ^^ao^ ^^. ' , '^ JUL 197 6 ^^ ^h RECE.IV ^ ^ ^; Volume 1 Apri 1 , 1976 `d ^^^ ^^t .^^+^' Number 4 Pub1 i shed by: The Astranamy Department ^8l ^ ^ b 4^'^ Box 4500, New Mexico Mate University Las Cruces, New Mexicfl 88003 This issue completes Volume 1. Future issues will bear the serial number onl,^, starting with the Number ^. ^ k ^ct`^^^c^^T' ^ w ^-, Z rn G ,^ tij a ^ERS o CONTRIBUTIONS OF THE 0 B ^ E RVATO RY OF NEW MEXICO STATE UNIVERSITY lAS CRUCES, NEW MEXICO 88003 Volume 1 April, 19'6 Number 4 Published oy: The Astronomy Department Box 4500, New Mexico State University Las Cruces, New Mexico 88003 This issue completes Volume 1. Future issues will bear the serial number only, st^.rting with the Number 5. i ^ ^ ^ t CONTRIBUTTONS OF THE OBSERVATORY, NE^dI^^XTCO STATE UNIVERSTTY Volume 1, dumber ^ April 1976 TABLE OF CONTENTS Page Non-LTE Proi=ilex of Strong Solar Lines. 110 T. J. ScTzneeberger and H. .^. Beebe Emissivi'^ies and Detectability of the Pure Rotational Transitions oi• Molecular Hydrogen. 123 T. J, Schneeber^ger Photometry oi= R Coronae Borealis. 134 D. W. Datvsor, and E. ^'. Tedesco Intermediate-Band Photometry of Faint Standard Stars. 14.0 D. W. Da^vson Seyt'ert Galaxies --- A Study of Brightness Variation and Stel i ar Concentration . 143 D. W. Darvsora Testing ofi a Photoelectric Photometer I. Determination of Operational Parameters. 148 D. W, Dc^son rand E. F. Tedesco II. Observational Testing. la4 D. W. rDaaJSOn and E. '.^'. Tedesco Photometric Calibration_o-^ Planetary Photographs. 1a9 R. F'. Beebe i - Impravemertt o-F the Rhodes l6-inch Telescope on Tortu^a5 Mountain 7 64©mi T . C. W. Tombaugh The ^[ASA-NMSU Automated Meteor ^bseYwatory. : i66 - G, A. Harvey. - NASA.Langley Research Center J. Gaffey Now Mexico Sate llniversity - Measurements of ^3upiter `s Long:-Lived Features and C^Irrents, T76 _ E. ' J. Reese and R: F. Beebe. '^ i Published by: As^ronamy Department Box 4500, - New Mexico State University Las Cruces, New Mexi co"g$003 - - _. .. - .. , ^: .. ^ .. This -issue comple^es ` Vol ume l: Future issues will bear I±he serial number anZy, starting 4vi th liur^ber 5. - ;=! } ^.._^^ :, i a T. J. 5chne^berger and Id. A. Beebe a -; Depari:ment of Astronomy New Mex^ca State Un^vers^ty, has Cruces, N.^f. 880x3 I I I ! i } ^ is ^ ^ III. The Model A-^mosphere ^ .. .. .__. ^ .. ,- 3 ^ r 5. Altrock and Canfield ^ 1 974) / • (1969 ' • Athay and ^anfiald .. ' ' Li p sky and Avrett (1970) .. .. Lites (1973) ^ • • • - -adopt®d . ^ • ^ 3. ^ ' ^ .• .^ • .- ^kr^/sec) .,^ e •^ • ' . , s . ^ ' • • .^ • • .. • • • • • • e s 4 • • • ^ • 0. ^ 0. 500. 1000. 1500. H^km^ Fig. 1. Microturbulence models, velocity (km/sec) vs. height (km). Neight is defined as in the HSRA. The adapted model follows Lites' in the photosphere and low chromosphere, and is the joined via the dashed line to the Li p sky-Avrett model. 114 t i { ^ i' ^ t ^ ^_ ^ ^ ^ ` - _ _ ^ ^ t 'i r ^ i - \ 1 _l ci Ca ^I 'three bevels pl us a continuum were included in the Ca r^ model, The bound levels are 4s ZS^fz' 3d 2 D5 f2 and 4p 2 P3/z . Detailed calculations ° ° were made i=ar the [^ 7 i ne, 393.0 A, the infrared tripl et ^ i ne at $452.7 A, and the 4s 25If2 -^ continuum transition. R v -^ dapendence was assumed for the rantinuum transition, and the pha^aianizatipn crass sect=on at the. coati nuuni- head +gas taken to be 7.1 x l 0^' 1 ' cm2 . The remaining ^ ^ ee-bound continaa were co^npute^ with fired rates; with TRRD = 5G00°K. The phatow ionization cross sections and coli%sionaT - crass sections were adopted from Auer, Heasley, and Mlkey (1.972). The Van der Waals dispersion constant for bath line transitions-was set at l.3 x 10 -32 ^Weideman, 1955}. ____e } ^^__^ z The h and k l i nes of Mg I i were cal cul aced i ^ detai 1 uti'^ i zi ng the model atom ar^d atomic data of Mi lkey and hlihalas X1974). This model includes the 3s zS^1Z' 3p Zp ^fz , 3p and can^it^uUm levels. Fixed zP°9f2 ti I I ^^ ^(a I X5890., Ca I ^9-227., Mg I A5172., Ca II X3933., and Ca II x8542., _ respectivEly, at disk center. The cores of i;he D 2 , 1t422T, and b 2 transitions are forr^^ed i n the 1 borer chrbmasphere. The line center optical depths, T o , become usual to unity for these transitions at te^iperatures and heights abode the temperature minimum. We have ' 0 (5890} = 1 at THSRA = 5200°K, ^e o (4227} = 1 at TNSRA 5000°K and zQ (5172) ^ 1 at TBSRA = 4700°K. The computed cores of these lines are darker than observed. It is well known that the microturbulent velocity gradient can effect the core brightness of lines and preliminary calculations with Ca i indicate that a microturbulence model with a steep gradient similar to that used by Altrock and Canfield {1.974) (see Figure 1) wi 17 produce the observed .core i n-^ensi ty of 1:4227.. at ^ ► l _0. The computes! Doppler cores _are wide compared to observations for both Ca I and.. Mg I. The wings of DZ , X4227., and b 2 are in reasonable agreement with observation Tests with Mg i X5172 have shown that the agreement can be 3 . e_ _ _ . ___.^.____e_ _r _ __._^^_ ^_.__.Y _^._._ 1L_ tl_._ .1 _._ 1.1 ..... 'l ... 1 .8 .a ^^ ,4 .2 0 .1 .2 .3 .^4 .5 ^ ,2 ,4 .6 ,8 1.0 n A a a► '.^ - ^ Fig. 2. pbserved (dashed) and computed {solid) profiles of tla [ 45090., Fig. 3, p6served (dashed} and computed {solid} profilos of Ca 1 x4227., ;:^ where I^ is Lhe ratio of tine to continuum intensity, at disk center. where I, is the ratio of lfrse to continuun intensity, at disk center. 3 i ,a I ^ l ^ i ,35 .d ii ^^ ,4 ^^ .10 .2 ,43 - 1 ^' r ,2 ,d .6 ,8 - 1.0 '.i 1 ^A .1 ,2 ,3 .,^ Fig. 4. Observed (dashed} and cnr^uted (solid) profiles of Mg [ 7,51'2., ^^ where I * 1s the ratio of lino to centinwrn intensity, at disk center. Fig. 5, p hsorved {dashed} and computed (solid} profiles of Ca II x3933., where T„ is the ratio of ilne to tontinumo intensity, at disk center. _. 119 .^ ! . _...... __. ^ 3 ^^ Figure 6 displays the results for the 78542 transition of Ca II. This line is not expected to show strong coherency effects. The Doppler care is in good agreement with observation, but the wing is tnn bright. This may be due to the collisinnal broadening parameters we have used. 9 We compare in Figure 7 our calculated Mg II J^2795 profile to the :1 computed profile obtained by Milkey and Mihalas (1974) in the complete ^ y redistribution case. Comparision with observations is, as with Ca Ii K, poor but the comparison does provide a consistency check. The differences ^ between the two calculations are smal7 k and are due mainly to the choice ^ l of a mic^,oturbulence model. Again, as with Ca II, partial redistribution ^ effects rrEay be Important for the Mg II h and k lines. ^^ The -transitions we have calculated in detail represent a wide range in core formation heights and wavelength. The results of this study provide a background for calculations which account explicitly for the ^ i inhomogerenusstructure of the chromosphere. The resulting two component chromosphere will then be restrained by this grid of line profiles. ', VI. Acknowledgments The authors wish to thank Dr, R. W, Milkey for helpful discussions. The assistance of the H.M.S.U. Computer Center staff is gratefully acknowledged. This work was supported by NSF Grant Ian. Lp-43815. `^ l 20 ^' ^ i r ^ r ^ ^ ^ ., f r ^ ~ r • ^* ,d ^f • ,^ ,^ ,C1 ^^ ] ® /► . - Fig. G. U6served (dashed} and computed (solid} profiles of Ca II a854Z., t^ihere I^ is the ratio of line to continuum intensity, at disk center. O i e 1 ^ ^ .1 .2 .3 ,4 ,5 ^^ Fig. 7. the results of Milkey and Mihaias (1974) with complete redistribution (dashed) and the profile computed in this study (solid) far Mg II aZ852., where I is intensity x l0' in ergs/cm^/sec/star /Hz at dis^C center.
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