Julie Hollek and Chris Lindner
Background on HK II Stellar Analysis in Reality Methodology Results Future Work Overview
Part of the HK Objective Prism Survey (Beers, Preston, Shectman 1985) Looked for low metallicity stars Used Ca II H and Ca II K lines as a metallicity indicator Observed as part of Chemical Abundances of Stars in the Halo (CASH) Project Characterize the abundance pattern of the galactic halo R~15,000 S/N ~50/1
Spectroscopically determined parameters Measure equivalent widths of known lines ▪ e.g. Fe I, Fe II Demand all abundances are the same from all lines Stellar Analysis
Demand no trend between excitation potential and abundance Gives temperature
Stellar Analysis Demand no trend between equivalent width and abundance Gives “correct” microturbulence
Stellar Analysis Demand ionization balance to determine the gravity For example, demand the same abundance for Fe I and Fe II to determine correct value for surface gravity
Stellar Parameters: Teff =5200 K log g =2.15 [Fe/H] = ξ = 2.0 Carbon, r+s -process, and lithium enhanced Most metal-poor Li enhanced star known to date
Li burns at 2.5x10^6 K Should be heavily depleted by the giant stage Li enhancement calls for some mechanism to produce more Li Extrinsic ▪ Binary companion Intrinsic ▪ Cameron-Fowler Beryllium Transport Mechanism ▪ Thermohaline Mixing Motivation
By determining the stellar evolutionary state of this star, we can determine its enhancement mechanism. Motivation
Changes in stellar parameters result in radically different line profiles Result from Voigt profile Example: change in Teff of 200 K of Li region Motivation
Observations of low metallicity candidates Change Teff and log g according to stellar evolutionary models (Girardi et al. 2000) Track how the Teff and log g change the line profile of a specific region in the spectrum Try to “match” observations Project Outline
Stellar Evolution Tracks Used model (Girardi et al. 2000) for star of Z = 0.01 and M = 0.8 Msun Models given as time steps with changes in luminosity, gravity, and effective temperature expressed
Stellar Analysis With approximate values for the stellar parameters of Teff, log g, [Fe/H], and ξ, we can create model atmospheres in a program such as TLUSTY or using Kurucz grid point models. We then input these stellar atmosphere models into a spectral synthesis program, like SYNSPEC or MOOG to model specific spectral features
SYNSPEC
TLUSTY
Kurucz Models LTE model atmospheres Using statistical opacity distribution function (ODF) of ~10^6 lines Monte-Carlo-like sampling of frequency points (Dreizler) Convection is available, though not used HK II is a low metallicity star, without the opacity source required for convection
Abundance Analysis MOOG Performs spectral synthesis Requires model atmosphere, line list, and observed spectrum
Results
As log g decreases, the lines get narrower As Teff decreases, the lines get stronger (deeper for a given abundance) Discussion of results Teff = 5900 K log(g) = 4.75Teff = 5200 K log(g) = 3.00 Teff = 4400 K log(g) = 1.00
Only low resolution observations exist These abundances are assumed to be constant over the lifetime of the star Probably change Stellar evolution tracks aren't exactly correct for the star Caveats
More observations for HK II are in the HET queue Detailed abundance analysis in the works Pb C12/C13 ratio Future Work