COOL STARS and ATOMIC PHYSICS Andrea Dupree Harvard-Smithsonian CfA 7 Aug. 2006 High Accuracy Atomic Physics In Astronomy
Dec 19, 2015
COOL STARS and ATOMIC PHYSICS
Andrea Dupree
Harvard-Smithsonian CfA 7 Aug. 2006
High Accuracy Atomic PhysicsIn Astronomy
OUTLINEHow does atomic physics influence our understanding of the atmospheres of cool stars ???
Three critical examples:1. Identifications temperatures2. Wavelengths dynamics3. Coll. X-sections densities Will draw from highly ionized species characteristic of
10MK, to singly ionized atoms observed in cool star spectra….
S
Giant stars
SupergiantsCool , extended
Solar type
Identification of Ions allows EMD
Emission Measure distributions quite different from the well-known solar case (Sanz-Forcada et al. 2004)
Highly Ionized Species FUSE spectra of cool stars show Fe XVIII at 974.86A.Identified in solar flare spectra.
Feldman and Doschek 1991Young et al. 2001Dupree et al. 2003Redfield et al, 2003.
Radial Velocity of Fe XVIII emission lines …
Reveals coincidence of Fe XVIII with the stellar photospheric velocities ,
Suggests that high T plasma,6.8 K (dex) is anchored closeto the stellar surface reminiscentof low-lying coronal loops…
High Temperature Species Anchored in Warm Wind
Fe XVIII
Fe XIX
FUSE Cool Star Team;Redfield et al. 2003
Symbiotic Star: AG DraThis stellar system consists of a red giant whose wind and surroundingnebula is photoionized by a hot white dwarf companion. Spectrum is complex with narrow nebular emission, and the surprising presencs of high ionizationforbidden lines. These conditions are quite different from ‘coronal’ plasmas(collisionally-dominated).
HST/STIS spectra revealforbidden lines: Ca VII, Fe VII, Mg V, Mg VI, Si VII, and for the first time,2 transitions of Mg VII between termsof the 2s 2 2p 2 3P-1D configuration(Young, P. et al. 2006).
Energy levels and density diagnostics
Separation of ground 3P levels(from IR astronomical spectra)plus UV wavelengths define 1D energy levels in Mg VII
Four density diagnostics usingMg ion ratios do not give consistent results,although the electron density appears to be high.High ionization appears to require nearby sourceof photoionization. Other problems remain that might be resolved by detailed modeling.(Young et al. 2006)
EUV spectra offer many coronal diagnostics
Spectra from the EUVE satellite contain ionsFe IX-XXIV (not FeXVII)allow both T and Ne tobe defined in cool star coronas.
(Sanz-Forcada et al. 2003)
Density diagnostics suggest small coronal structures
Electron densities are high.The observed line flux in combination with the densitydiagnostic suggest small emitting volumes (<0.01 R)and continuous heating.
FLUXobs ~ Ne 2 ΔV
Sanz-Forcada et al. 2004
EUV radiance spectrum of the Sun
CHIPS EUV spectrum of the whole Sun revealsdifferences from the standard solar irradiance models (red line).
Courtesy of M. Hurwitz(2006)
Fluorescent processes in extended atmospheres
Narrow lines appeared in emission in far UV (ORPHEUS) spectra of cool giants and supergiants near 1140Ǻ. Possibly fluorescentlines from low ionization species.
Dupree and Brickhouse 1998Betelgeuse – a supergiantImaged in the ultraviolet by HST
Higher resolution led to confirmation
Fe II can be produced by H-Lyman-α pumping from4s a4D and cascade to 4s a6D and 3d7 a4F.May provide an indirect diagnostic of stellar Lyman-α profile .Harper et al (2004) hypothesized that Fe II lines away fromH-Ly α (Δλ > 1.8Ǻ) should be weak (marked by *).
FUSE Spectra show puzzling differences
FUSE spectra of luminous stars do not show consistent patterns.(Dupree et al. 2005)
Unresolved Problem: C III profiles
Profiles of the C III 1176Ǻ line3P-3P, in luminous cool stars differsubstantially from the solar profile.Check center to limb behavior.
(Dupree et al 2005)