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[ {6" \ {6# ] {6$ ^ {63 _ s sv64 ` ss65 a {s66 b {67 c {68 d {6: e 6; f s s6< g s6= h {s6> i {s6? j {6@ k {5eV!5dq5;PFe5dq6LH'5dq7s8CF5Hm3R q897 Hm3R H RH R FootnoteHr@ q98:7 Hr@ HzHz  Single LineRH'q:9<7 s;;Footnote  5_;:t     HD q<:=7 6 HD HH  Double LineH q=<@763>?s Double Linea 5c>?=5e?>=6=6> H q@=B7AA Single Line;5hA@HZqB@C7q TableFootnoteEGxR qCB7 9EGxR EPwEPw  TableFootnoteod5pDRRHH5xE5 HH Fe   HH5zFN5 HHlEE HH5{G6 HH @>?HDoe   HH5}HJ6HHlGG HUV 5~I6 HUV AAJUU`   HUV 5JLH6HUV lII H$ 5K6 FtnH$ ELUU` tn oH$ 5LJ6H$ lKK HUV 5M5 HUV N UUe !  HUV 5NPF5HUV lMM H$ 5O5 H$ P UUe "  H$ 5PN5H$ lOO HH5QD HH8A((R ( ` # 79205 Astronomy Fall 1996 UT UT` $ +Some practice questions for the final exam .` %  < & h1.  HR diagrams of stars in our Galaxy show many stars with absolute magnitude  M 2.0  and J@ & Jobetween  K  and  M  spectral types. In the center of these stars, the dominant nuclear process is 5X` ' UV A. Hydrogen burning into helium f` ( B. Hydrogen burning into carbon t` ) C. Helium burning into carbon ` * D. Carbon burning into silicon MM` 4 E. Silicon burning into iron ` .   - c2.  You want to resolve the shape of an HI region in a galaxy using a 100 m diameter radio tele@ - Tscope. If the region is 10 kpc in diameter, the galaxy can be no farther away than ` / A. 10 kpc ` 0 B. 1 Mpc ` 1 C. 5 Mpc ` 2 79 D. 100 Mpc Fa` 3 Ȫ E. 1000 Mpc p` 5 fo h 6 i3.  A stars visible magnitude is 0.56 brighter than its blue magnitude. Assuming the star is on the s*@ 6 Tmain sequence and ignoring interstellar reddening, its spectral type is most likely es8` 7 f A. B0 F` 8 nuB. A0 T` 9 C. F0 b` : buD. G0 p` ; E. K0 ~` < bu n` = S4.  A billion years from now, the Hubble constant, compared to today, will be ng ` > A. Larger ` ? ur B. Smaller n ` @ C. The same ` A ou?D. It depends on whether the universe is open, closed, or flat 0 m` B leFE. The answer depends on details of the inflation theory of cosmology ` C o  t` D Y5.  The mechanism by which a nova increases its brightness is most closely related to ` E 79A. Cepheid pulsation  ` F 00*B. Solar flare-type events on large stars ` G sC. T Tauri stars t&` H erD. Type I Supernovae e4` I arE. Type II Supernovae HH5RDtlaHHlUQQ ` 7d5SUUHH5TS HHJ**A billiUno*` ,  r J bef6.  The density wave theory of spiral galaxies predicts that vigorous star formation occurs in the $ J Abspiral arms. Which of the following wavelength bands is therefore best used to show spiral struc2@ J d"ture in a  distant  galaxy? @` K A. Blue tN` L B. Red The\` M h C. 21 cm radio itsj` N t D. Continuous radio x` O A. E. X-ray l` P  F Q reh7.  A star cluster in our Galaxy is shown to consist mostly of main sequence stars. An F5-type star ov Q Ipin the cluster has an apparent magnitude of  m =8.0 . Ignoring interstellar reddening, the distance to @ Q the cluster is most likely S` R A. 1.0 pc ` S B. 10 pc ` T C. 40 pc ` U D. 200 pc ` V * E. 2 kpc ` W * ` Y *V8.  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