000005490 001__ 5490
000005490 005__ 20211217085934.0
000005490 0247_ $$2DOI$$a10.1051/0004-6361/202141473
000005490 037__ $$aSCART-2021-0150
000005490 100__ $$aMehner, A.
000005490 245__ $$aLBV phenomenon and binarity: The environment of HR Car
000005490 260__ $$c2021
000005490 520__ $$aLuminous blue variable stars (LBVs) are of great interest in massive-star evolution as they experience very high mass-loss episodes within short periods of time. HR Car is a famous member of this class in the Galaxy. It has a large circumstellar nebula and has also been confirmed as being in a binary system. One means of gaining information about the evolutionary status and physical nature of LBVs is studying their environments. We investigated the stellar content within ∼100 pc of HR Car and also its circumstellar nebula. Very Large Telescope Multi Unit Spectroscopic Explorer (MUSE) observations of a 2'×2' region around the star highlight the incompleteness of stellar classification for stars with magnitudes of V > 13 mag. Eight B0 to B9 stars have been identified which may lie in close spatial vicinity to HR Car. For a region with a radius of r = 1.2° (∼100 pc at a distance of 4.8 kpc) around HR Car, existing catalogs list several late O-type and early B-type stars, but only one early O-type star. Given the relatively low stellar and nebular masses in the HR Car system, no early O-type stars and only a few late O-type stars would be expected in association with HR Car. Instead, HR Car's location in a point vector diagram suggests that HR Car is not isolated, but is part of a moving group with a population of B-type stars in a spiral arm, and it has not received a strong kick from a supernova explosion of a companion star or a merger event. Potential binary evolution pathways for the HR Car system cannot be fully explored because of the unknown nature of the companion star. Furthermore, the MUSE observations reveal the presence of a fast outflow and "bullets" that have been ejected at intervals of about 400 years. These features may have been caused by recurrent mass transfer in the system.
000005490 594__ $$aNO
000005490 700__ $$aJanssens, S.
000005490 700__ $$aAgliozzo, C.
000005490 700__ $$ade Wit, W. -J.
000005490 700__ $$aBoffin, H. M. J.
000005490 700__ $$aBaade, D.
000005490 700__ $$aBodensteiner, J.
000005490 700__ $$aGroh, J. H.
000005490 700__ $$aMahy, L.
000005490 700__ $$aVogt, F. P. A
000005490 773__ $$c10$$nA33$$pAstronomy & Astrophysics$$v655$$y2021
000005490 8560_ $$flaurent.mahy@ksb-orb.be
000005490 8564_ $$s4671434$$uhttp://publi2-as.oma.be/record/5490/files/Mehner2021_HRCar.pdf
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000005490 8564_ $$s6511$$uhttp://publi2-as.oma.be/record/5490/files/Mehner2021_HRCar.jpg?subformat=icon-180$$xicon-180
000005490 905__ $$apublished in
000005490 980__ $$aREFERD