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The young B-star quintuple system HD 155448 | | O. Schuetz
; G. Meeus
; A. Carmona
; A. Juhász
; M. F. Sterzik
; | | Date: |
7 Aug 2011 | | Abstract: | Until now, HD 155448 has been known as a post-AGB star and listed as a
quadruple system. In this paper, we study the system in depth and reveal that
the B component itself is a binary and that the five stars HD 155448 A, B1, B2,
C, and D likely form a comoving stellar system. From a spectroscopic analysis
we derive the spectral types and find that all components are B dwarfs (A: B1V,
B1: B6V, B2: B9V, C: B4Ve, D: B8V). Their stellar ages put them close to the
ZAMS, and their distance is estimated to be ~2 kpc. Of particular interest is
the C component, which shows strong hydrogen and forbidden emission lines at
optical wavelengths. All emission lines are spatially extended in the eastern
direction and appear to have a similar velocity shift, except for the [OI]
line. In the IR images, we see an arc-like shape to the northeast of HD 155448
C. From the optical up to 10 micron, most circumstellar emission is located at
distances between ~1.0 arcsec and 3.0 arcsec from HD 155448 C, while in the Q
band the arc-like structure appears to be in contact with HD 155448 C. The
Spitzer and VLT/VISIR mid-IR spectra show that the circumstellar material
closest to the star consists of silicates, while polycyclic aromatic
hydrocarbons (PAH) dominate the emission at distances >1 arcsec with bands at
8.6, 11.3, and 12.7 micron. We consider several scenarios to explain the
unusual, asymmetric, arc-shaped geometry of the circumstellar matter. The most
likely explanation is an outflow colliding with remnant matter from the star
formation process. | | Source: | arXiv, 1108.1557 | | Services: | Forum | Review | PDF | Favorites | |
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