2MASS Two Micron All Sky Survey
a distance between star centers, “orbital separation”
a1, a2 distance from the center of the primary/secondary star to the center of gravity Ai surface area of a surface element
Ai(φ) projected surface area of a surface element
∆Ai accumulated change of the projected surface area of the i-th surface element ADS Astrophysics Data System
B magnetic field strength
c speed of light, c= 299 792 458 km s−1 CV cataclysmic variable binary star CVcat catalogue of CVs
CVMOD CV model code of this work d, d0 number of dimensions
Di default image intensity of the i-th surface element DBI/DBD database interface/database driver
EM eclipse mapping
EUVE Extreme Ultraviolet Explorer FOEM full-orbit eclipse mapping
FWHM full width at half maximum, in case of a Gaussian:
FWHM= √
8 ln 2·σ≈2.355·σ
F observed flux
Fλ observed flux at wavelength λ
FORS2 FOcal Reducer/low dispersion Spectrograph at the VLT FOS Faint Object Spectrograph on the HST
G gravitational constant, G = 6.672 59(85)·10−8cm3g−1s−2 GHRS Goddard High Resolution Spectrograph on the HST HIT High Time Resolution modes for FORS2
119
HST Hubble Space Telescope HTML Hypertext Markup Language HTTP Hypertext Transfer Protocol
i inclination
i, j counters
~I vector holding all surfaces’ intensities Ii intensity of the i-th surface element
Ii,λ intensity of the i-th surface element at wavelength λ K amplitude of the orbital velocity variation
L1 inner Lagrangian point
m number of reconstructed dimensions M total system mass
M1, M2 primary/secondary mass M solar mass, M = 1.989e33 g
r distance from the center of the magnetic dipole
r1, r2 distances from the primary/secondary star to a given position (x, y, z) R radius of a star
TWIN two channel spectrograph at the 3.5 m Calar Alto telescope
v velocity
V velocity derived from the Doppler shift of a spectral line V visible surface area
V(φ) set of the visible surface elements at phase φ
UV ultraviolet
VLT Very Large Telescope at Cerro Paranal VLTI Very Large Telescope Interferometer
121 VLT UT2 Telescope #2 of the VLT
VSNET Variable Star Network
WD white dwarf
x, y, z spatial positions
˙
x,y,˙ z˙ velocities
¨
x,y,¨ z¨ accelerations
α angular size
α angle between the dipole axis and a position β dipole axis tilt
∆ smooth width for the default image calculation γ systemic velocity
λ wavelength
λ parameter controlling the contribution of the entropy to the quality of a fit µ (M1+M2)/M1, inverse mass fraction of the primary star
ϕ angle around the dipole
φ orbital phase
φ0 phase offset
Φ Roche potential
Ψ dipole axis azimuth
ΨS azimuth of the stagnation region
σ standard deviation or width parameter of a Gaussian (see also FWHM) χ2 sum of squared residuals
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