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Table 1

Stellar and wind parameters obtained from line profile fits of observations taken in Arizona in 2013.

Date JD Teff log  g β v vmacro(Hα) R log  L/L
dd/mm/yr [K] [cgs] [10-6M yr-1] [km s-1] [km s-1] [R]

17/10/2013 2 456 582.72 19 000 ± 400 2.50 ± 0.1 2.0 0.295 ± 0.01 310 ± 30 50 ± 5 58 ± 1 5.60 ± 0.03
18/10/2013 2 456 583.70 19 000 ± 400 2.50 ± 0.1 2.0 0.295 ± 0.01 310 ± 30 20 ± 5 58 ± 1 5.60 ± 0.03
19/10/2013 2 456 584.62 19 000 ± 400 2.50 ± 0.1 2.0 0.310 ± 0.01 320 ± 30 35 ± 5 58 ± 1 5.60 ± 0.03
20/10/2013 2 456 585.67 19 000 ± 400 2.47 ± 0.1 2.0 0.320 ± 0.01 320 ± 30 50 ± 5 57 ± 1 5.59 ± 0.03
21/10/2013 2 456 586.73 19 100 ± 400 2.50 ± 0.1 2.0 0.280 ± 0.01 300 ± 30 60 ± 5 57 ± 1 5.60 ± 0.03
22/10/2013 2 456 587.70 19 000 ± 400 2.40 ± 0.1 2.0 0.285 ± 0.01 310 ± 30 60 ± 5 58 ± 1 5.60 ± 0.03
23/10/2013 2 456 588.59 19 000 ± 400 2.40 ± 0.1 2.0 0.285 ± 0.01 350 ± 35 60 ± 5 58 ± 1 5.57 ± 0.03
25/10/2013 2 456 590.59 18 650 ± 400 2.40 ± 0.1 2.0 0.190 ± 0.01 300 ± 30 40 ± 5 58 ± 1 5.57 ± 0.03
26/10/2013 2 456 591.59 18 600 ± 400 2.40 ± 0.1 2.0 0.180 ± 0.01 270 ± 30 50 ± 5 57 ± 1 5.55 ± 0.03
27/10/2013 2 456 592.59 18 570 ± 400 2.40 ± 0.1 2.0 0.170 ± 0.01 270 ± 30 50 ± 5 56 ± 1 5.53 ± 0.03
28/10/2013 2 456 593.60 18 570 ± 400 2.40 ± 0.1 2.0 0.170 ± 0.01 270 ± 30 40 ± 5 56 ± 1 5.53 ± 0.03
30/10/2013 2 456 595.71 19 000 ± 400 2.36 ± 0.1 2.2 0.284 ± 0.01 330 ± 30 40 ± 5 57 ± 1 5.58 ± 0.03
31/10/2013 2 456 596.71 18 600 ± 400 2.40 ± 0.1 2.0 0.180 ± 0.01 270 ± 30 60 ± 5 57 ± 1 5.55 ± 0.03
01/11/2013 2 456 597.57 18 600 ± 400 2.40 ± 0.1 2.0 0.175 ± 0.01 260 ± 30 60 ± 5 57 ± 1 5.55 ± 0.03
07/11/2013 2 456 603.59 18 570 ± 400 2.40 ± 0.1 2.0 0.170 ± 0.01 270 ± 30 40 ± 5 56 ± 1 5.53 ± 0.03

Notes. Listed are the date of observation, the Julian date (JD), the derived effective temperature (Teff) and log  g, the β exponent of the velocity law, the mass-loss rate (), the terminal velocity (v), the macroturbulent velocity in Hα (vmacro(Hα)), the stellar radius (R), and the luminosity (L). Mass-loss rates are for smooth wind models.

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