List B

This list includes objects deserving some caution regarding their membership to the class of particle-accelerating colliding-wind binaries, even though these objects have been suspected (or even claimed) to belong to this class. Future investigations on some of these objects may lead to a change of their status, possibly allowing them to be moved to List A. This list also includes a few former members of list A that were removed after further investigation.

The list is structured as follows:
Col.1 : Number of the object in the catalogue (the numbers are dynamically updated when new objects are included)
Col.2 : Identifier, with hyperlink to the individual sheet
Col.3 : Alternative identifiers
Col.4 : Right ascension (2000)
Col.5 : Declination (2000)
Col.6 : Spectral types
Col.7 : Comment



CC Cas HD1982003 14 05.34+59 33 48.48O8.5III + B0VPossible eclipse-like variation


xi PerHD2491203 58 57.90+35 47 27.71O7.5III (or I) + ?Runaway star


alpha CamHD3061404 54 03.01+66 20 33.64O9.5IRunaway candidate


delta Ori C HD3648505 32 00.41–00 17 04.46B2VMagnetic Bp star


theta1 Ori AHD3702005 35 15.85–05 23 14.34B0.5V + TT + ?Presence of a T Tauri component


HD37017HR189005 35 21.87–04 29 39.02B1.5IV + ?Magnetic Bp star


sigma Ori EHD3747905 38 47.19–02 35 40.54B2VMagnetic Bp star


WR22HD9274010 41 17.52–59 40 36.90WN7 + O9Spectral index not accurate


WR79HD15227016 54 19.70–41 49 11.54WC7 + O5-8Possible source confusion


WR86HD15632717 18 23.06–34 24 30.63WC + OBSpectral index not accurate


W43 #1–18 47 36.69–01 56 33.06WR? + ?Possible phenomena combination


HD 190603BD+31 392520 04 36.18+32 13 06.95B1.5IaFlat index more typical of optically thin


Cyg OB2-11BD +41 380720 34 08.52+41 36 59.36O5I(f)NT status uncertain


WR156HIP11356923 00 10.12+60 55 38.42WN8h + OBNT status uncertain
Individual sheets can be accessed by clicking the highlighted identifers. The individual sheets contain many information on the catalogue members, including relevant references whose details are given in the bibliography.

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