8. * ** =

15. SUMER spectra

16. Continuum measurements 1 st - order = 1350 Å, 2 nd -order = 675 Å 1 st- and 2 nd -order continuum near Fe XII 2 nd -order continuum near C II 2 nd - order more apt to be absorbed by H I Ratio of 1 st -to-2 nd -order cont. shows location of absorption

17. Time-space “stackplots”

18. Dark in emission lines  not “hot + dense”

19. Continuum ratio maps (3.5 x 1 st -order  2 nd -order) (bremsstrahlung  ratio=1)

20. Binaries Visual binary (VB) – see both stars Astrometric binary (AB) – see one, but it “wiggles” Spectroscopic binary (SB) – see one, but line-of-sight velocity oscillates Eclipsing binary (EB) – light curve

21. SB: Splitting or shifting of spectral lines “single line”, one star much brighter than the other, compare shift to local calibration lamp “double line”, see spectrum from both stars Radial velocity v =  c / 0 “double line”  ratio of v 1 /v 2 yields M 2 /M 1 If (R+r)/a  cos(inclination), then  EB

22. Fake simple eclipse Deeper “primary” eclipse is when the hotter star is hidden A flat bottom to the eclipse indicates that the star is completely obscured Time in eclipse, as fraction of the total period, yields info about relative sizes, separation, even tidal bulge

23. Example: oblate spheroid with a tidal bulge

24. Example: brightening around secondary minimum? Answer: brighter star reflects off the fainter star

25. If you can observeThen you can computeIf also knowThen (1a) Apparent orbit of VB, relative only P, a”, e,  incl. ”” a, M 1 + M 2 (1b) Apparent orbit of VB, center-of-mass P, a 1 ”, a 2 ”, e,  incl. ”” a 1, a 2, M 1, M 2 (2) Light curve of EBP, incl., R 1 /a, R 2 /a, relative temp. (3a) Radial velocity of SB, single line P, (a 1 sin(incl.)), e (3b) Radial velocity of SB, double line P, (a 1 sin(incl.)), (a 2 sin(incl.)), e P = period a” = semimajor axis of relative orbit (arcsec) a = semimajor axis of absolute orbit (a.u., or pc)  ” = parallax (arcsec)