The rotation of the primary of Algol

Tomkin, J.; Tan, Huifeng

doi:10.1086/131493

Cited by 4 publications

(1 citation statement)

References 8 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Moreover, the direction of the flow in the V z direction in β Per was opposite to that in RS Vul. In both binaries, the projected rotational velocity, v sin i is comparable to the synchronous rotational velocity of the mass gainer (50 -60 km s −1 ), and both are lower than the maximum V z (adj) velocities associated with this feature (e.g., v sin i = 53 ± 3 km s −1 for β Per; Rucinski 1979;Tomkin & Tan 1985). Since the V z (adj) velocities associated with Feature 1 are higher than the star's rotational velocity, it is reasonable to assume that the star may have been spun up, presumably by the impact of the gas stream onto the stellar photosphere.…”

Section: Description and Interpretation Of Emissionmentioning

confidence: 82%

New Evidence of Magnetic Interactions Between Stars From Three-Dimensional Doppler Tomography of Algol Binaries: Β Per and Rs Vul

Richards

Agafonov

Шарова

2012

ApJ

View full text Add to dashboard Cite

Time-resolved Hα spectra of magnetically-active interacting binaries have been used to create 3D Doppler tomograms by means of the Radioastronomical Approach. This is the first 3D reconstruction of β Per, with RS Vul for comparison. These 3D tomograms have revealed evidence of the mass transfer process (gas stream, circumprimary emission, localized region, absorption zone), as well as loop prominences and coronal mass ejections (CMEs) in β Per and RS Vul that could not be discovered from 2D tomograms alone. The gas stream in both binaries may have been deflected beyond the central plane by the mass losers magnetic field. The stream was more elongated along the predicted trajectory in RS Vul than in β Per, but not as pronounced as in U CrB (stream-state). The loop prominence reached maximum V z velocities of ±155 km s −1 in RS Vul compared to ±120 km s −1 in β Per, while the CME reached a maximum V z velocity of +150 km s −1 in RS Vul and +100 km s −1 in β Per. The 3D tomograms show that the gas flows are not symmetric relative to the central plane and are not confined to that plane; a result confirmed by recent 15GHz VLBI radio images of β Per. Both the 3D Hα tomography and the VLBI radio images support an earlier prediction of the superhump phenomenon in β Per: that the gas between the stars is threaded with a magnetic field even though the hot B8V mass gaining star is not known to have a magnetic field.

show abstract

Section: Description and Interpretation Of Emissionmentioning

confidence: 82%