HR 2142, thirty years after it was hypothesized fo be an interacting binary

Title:

HR 2142, thirty years after it was hypothesized fo be an interacting binary

Creator:

Peters, Geraldine J.

Identifier:

https://cdk.lib.cas.cz/client/handle/uuid:2f18c514-5f2e-488d-bdd8-554961d7e65b
uuid:2f18c514-5f2e-488d-bdd8-554961d7e65b

Subject:

Be stars, close binary stars, and stars: individual: HR 2142

Type:

model:article and TEXT

Format:

bez média and svazek

Description:

The corona status of our knowledge of the HR 2142 system is reviewed. The massflow in the system and its long-term behavior are currently being studied using IUE HIRES data obtained between 1979-95 and archival Copernicus observations acquired in the late 1970s. Some recent results are summarized here. The strength and velocity behavior of the infall components to the Si II, IV lines seen during the primary shell phase from φ ~0.70-0.98 resemble that observed in conventional Algol systems. The inferred mass infall rate of ~10^-7 M⊕ yr^-1, however, is too small to account for the massive Hα-emitting disk about the primary. The cause for the mass outflow observed during the secondary shell phase is still unknown. The nature of the secondary star, which remains undetected, is discussed. The small amount of residual flux in the UV that might be attributed to the secondary weakens the assumption that it must be an O subdwarf as in the φ Per system, but further studies are warranted.

Language:

Czech

Rights:

http://creativecommons.org/publicdomain/mark/1.0/
policy:public

Coverage:

[30]-35

Source:

Publications of the Astronomical Institute of the Academy of Sciences of the Czech Republic | 2001 Volume:89 | Number:89

Harvested from:

CDK

Metadata only:

false