New perspectives on B star X-ray emission: The high-resolution X-ray spectra of Spica and β Cen.

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Presentation transcript:

New perspectives on B star X-ray emission: The high-resolution X-ray spectra of Spica and β Cen

Collaborators on both projects: –Nathan Miller –Joe Cassinelli β Cen –Ton Raassen –Emre Tepedelenlioglu –Rolf Mewe Spica –Ron Reynolds –Joe MacFarlane –Nate Hall

Main Question: Where and how do B stars produce their X-rays? Three approaches: –Line profiles – broadened or not? –Line ratios from He-like ions –Is X-ray flux affected by β Cep-type pulsations

Stars’ Biographical Details Beta CenSpica Spectral TypeB1 IIIB1 IV Vinf (km/s) Mdot (Msun/yr)2.7x x10 -8 β Cep Period (d)0.157 d d SatelliteXMMChandra InstrumentRGS/MOS/PNACIS-S/LETG

β Cen XMM spectra

Spica LETG-ACIS-S spectrum

1. Emission Line Profiles

Profiles of CVI line of β Cen

Spica Line Profiles (vs. scaled Capella in red) (Capella Aa (the main X-ray source) had v ≈ +25 km/s during the observation shown here (Ishibashi & Dewey 2005)

2. f/i Ratios from He-like Ions

f/i ratios for β Cen (Kurucz model)

Spica’s Ne IX fir region

Spica’s O VII fir region

Density falloff in Spica’s wind Critical Densities Marked: Radiation will control f/i ratio

Interpreting Spica’s f/i ratios (Hubeny model)

Interpreting Spica’s f/i ratios (Kurucz model – calc by MacFarlane)

-H II region is relatively isolated -Will use to measure ionizing flux and calibrate photospheric FUV/EUV flux which effects f/i ratios Spica’s H II region (Wisconsin H-Alpha Mapper (WHAM) image)

3. X-ray Lightcurves

β Cen Lightcurves: 3 XMM instruments

β Cen – folded on β Cep period

Spica β-Cep-Type History Seen as β Cep variable by Shobbrook et al. (1969) with p= d (pulsations evident in archived observations) Photometric variations died out by 1972 (Lomb 1978) May still be pulsing, but axis of NRP may have processed so that we are observing pole-on (Balona 1985) (precession period yrs) (Dukes 1974)

Spica’s X-ray Lightcurve

Spica data folded on β Cep period

Conclusions: X-ray emission lines are not strongly Doppler-broadened in either case He-like ions indicate X-rays formed at a range of radii (at least for Spica) No evidence is found for either star to be variable in X-rays on their β Cep periods