IXO/CAT: Simulation: AB Dor
Simulations of AB Dor: detecting coronal Doppler signatures(D.Huenemoerder Nov 2008 firstname.lastname@example.org)
AB Dor is a rapidly rotating K0 dwarf with a strong corona. Here we investigate the possibility of detecting coronal spatial non-uniformities in line profile variability due to the rotational Doppler signature. AB Dor has rotational period of 0.5 days and a projected radial velocity of 93 km/s. It nearby (15 pc) and relatively bright in X-rays (3.5E-11 ergs/cm^2/s).
The model is comprised of a steady, uniform corona, with a superimposed idealized variable component which varies simusoidally in flux and velocity at the rotational period. The flux amplitude is 15% of the steady component, and the velocity amplitude is 90 km/s, which is the projected rotational velocity of the star.
We used a plasma model is based on Sans-Forcada et al (2003; A&A 408, 1087). The velocity model is loosely based on results in Hussain et al (2007, MNRAS 377, 1488).
Simulation OverviewSimulations were done with the Project quideline grating effective area of 3000 cm^2 and a resolving power of 3000, using our CAT response files.
This figure shows an overview of the spectral simulation for a 11 ks exposure. The black curve is from the zeroth order plus direct beam as detected by the microcalorimeter (XMS). The red is the CAT grating spectrum, detected by a grating readout.
The complementary nature of the combined instrument is more clearly seen in these figures:
The XMS has high efficiency and high resolving power at short wavelengths (below 10A; above 1.2 keV)
Above 10A, the CAT efficiency increases and the resolving power becomes larger than the XMS.
Here, at 13A, we can see the power of the grating spectrometer. Note the strong Fe blends in the Ne IX triplet at 13.5A.
Simulation Detail: O VIITo investigate the Doppler signature, we look at one line, O VII 21.6A, the resonance line in the He-like triplet. This figures gives an overview of the spectrum in this region.
To obtain phase sampling, we assumed that the total observation covered 5 stellar rotations, or 224 ks. Thus, in phase bins of 0.05, we have 11 ks exposure. These figures show the simulated O VII profiles from the CAT 3rd order for 11 ks in a phase bin of width 0.05 near phases 0.25 (left) and 0.75 (right). The black histogram is the simulated spectrum, and the red is a model of the steady component renormalized to match the line core. The Doppler signature of the variable compoenent is clear.
This animation shows the feature modulated in strength and velocity by rotation.
Simulation ScriptThis simulation was done in ISIS and used APED plasma models. The main simulation script is sim_abdor.sl. The initial plasma model is defined by this ISIS parameter file: AB_Dor_plaw_dem-1.par.
The script requires these utility files:
This page was last updated Jan 8, 2010 by David P. Huenemoerder. To comment on it or the material presented here, send email to email@example.com.