Stellar Winds of central stars of the LMC PNe
A. Arrieta1,
L. Stanghellini2
1Universidad Iberoamericana, Mexico
2NOAO, Tucson, AZ, USA
We analyzed UV spectra of twelve central stars of planetary nebula in
the Large Magellanic Cloud. The observations were made with HST STIS
in ultraviolet slitless spectroscopy mode, with gratings G140L and
G230L. The spectra of the central stars were extracted from the 2D image.
The high spatial resolution of HST allows separation of the nebular and
stellar spectra. Further correction to the stellar extraction is
provided by the nebular spectra themselves. The 1D spectra were then corrected
for the galactic and LMC extinction.
The stellar temperature and luminosities were derived by fitting the
stellar continua, and constraining the fitting procedure by using the
optical magnitudes derived from the optical HST data.
The nebular contribution to the continuum were estimated via CLOUDY
Some of the objects show P Cyg profile correspondent to the C IV
1548/1551 Å,
Si IV 1394/1403 ÅÅ and N V 1239/1243 ÅÅ lines.
We fit these lines using
a line
transfer code together with a genetic minimization algorithm. We report
the obtained mass loss rates and terminal velocities.
A comparison from our results with the ones obtained by other groups
for central stars in Galactic planetary nebula is discussed.