J/A+A/618/A110 IR nebulae around bright massive stars (Bodensteiner+, 2018)
Infrared nebulae around bright massive stars as indicators for binary
interactions.
Bodensteiner J., Baade D., Greiner J., Langer N.
<Astron. Astrophys. 618, A110 (2018)>
=2018A&A...618A.110B 2018A&A...618A.110B (SIMBAD/NED BibCode)
ADC_Keywords: Stars, early-type ; Stars, emission ; Stars, Be ;
Rotational velocities ; Stars, double and multiple ;
Diffuse clouds ; Nebulae
Keywords: stars: early-type - stars: emission-line, Be - stars: rotation -
binaries: general - circumstellar matter - dust, extinction
Abstract:
Recent studies show that more than 70% of massive stars do not evolve
as effectively single stars, but as members of interacting binary
systems. The evolution of these stars is thus strongly altered
compared to similar but isolated objects. We investigate the
occurrence of parsec-scale mid-infrared nebulae around early-type
stars. If they exist over a wide range of stellar properties, one
possible overarching explanation is non-conservative mass transfer in
binary interactions, or stellar mergers. For ∼3850 stars (all OBA
stars in the Bright Star Catalogue (BSC, Cat. V/50), Be stars, BeXRBs,
and Be+sdO systems), we visually inspect WISE 22um images. Based on
nebular shape and relative position, we distinguish five categories:
offset bow shocks structurally aligned with the stellar space
velocity, unaligned offset bow shocks, and centered, unresolved, and
not classified nebulae. In the BSC, we find that 28%, 13%, and 0.4% of
all O, B, and A stars, respectively, possess associated infrared (IR)
nebulae. Additionally, 34/234 Be stars, 4/72 BeXRBs, and 3/17 Be+sdO
systems are associated with IR nebulae. Aligned or unaligned bow
shocks result from high relative velocities between star and
interstellar medium (ISM) that are dominated by the star or the ISM,
respectively. About 13% of the centered nebulae could be bow shocks
seen head- or tail-on. For the rest, the data disfavor explanations as
remains of parental disks, supernova remnants of a previous companion,
and dust production in stellar winds. The existence of centered
nebulae also at high Galactic latitudes strongly limits the global
risk of coincidental alignments with condensations in the ISM. Mass
loss during binary evolution seems a viable mechanism for the
formation of at least some of these nebulae. In total, about 29% of
the IR nebulae (2% of all OBA stars in the BSC) may find their
explanation in the context of binary evolution.
Description:
We investigate the surroundings of ∼ 3850 stars (all OBA stars in the
Bright Star Catalogue (BSC, Cat. V/50), Be stars, BeXRBs, and Be+sdO
systems) in WISE 22 micron images.
For all stars we find associated with extended IR nebulae we gather
stellar parameters from the literature, including identifiers,
coordinates, HD number, V-band magnitudes, spectral types from SIMBAD.
Additionally we give Hipparcos parallaxes and Hipparcos proper motions
(van Leuwen, 2007A&A...474..653V 2007A&A...474..653V, Cat. I/311) when available. Proper
motions are converted to the rest frame of the local ISM by correcting
for the Galactic rotation (Comeron & Pasquali, 2007A&A...467L..23C 2007A&A...467L..23C).
Radial velocities are collected mainly from Gontcharov
(2006AstL...32..759G 2006AstL...32..759G, Cat. III/252), but also from Kharchenko et al.
(2007, Cat. J/AN/328/889) or Pourbaix et al. (2004A&A...424..727P 2004A&A...424..727P,
Cat. V/122).
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tableb1.dat 114 255 Compilation of all parameter values from the
literature
tableb2.dat 120 255 Overview over all the measured and calculated
parameters
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See also:
V/50 : Bright Star Catalogue, 5th Revised Ed. (Hoffleit+, 1991)
I/311 : Hipparcos, the New Reduction (van Leeuwen, 2007)
III/252 : Pulkovo radial velocities for 35493 HIP stars (Gontcharov, 2006)
V/122 : SB9: 9th Catalogue of Spectroscopic Binary Orbits (Pourbaix+ 2005)
Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Name BSC Identifier of the star
14- 15 I2 h RAh Right ascension (J2000.0)
17- 18 I2 min RAm Right ascension (J2000.0)
20- 24 F5.2 s RAs Right ascension (J2000.0)
26 A1 --- DE- Declination sign (J2000.0)
27- 28 I2 deg DEd Declination (J2000.0)
30- 31 I2 arcmin DEm Declination (J2000.0)
33- 36 F4.1 arcsec DEs Declination (J2000.0)
38- 43 I6 --- HD HD identification number
45- 49 F5.2 mag Vmag Apparent V-band magnitude
50- 64 A15 --- SpType Spectral classification listed in SIMBAD
67- 71 F5.2 mas plx ?=-9.99 Parallax (1) (2)
73- 77 F5.2 mas e_plx ?=-9.99 Parallax error (1) (2)
79- 84 F6.2 mas/yr pmRA Proper motion in RA (1)
86- 90 F5.2 mas/yr e_pmRA ?=-9.99 Proper motion error in RA (1)
92- 97 F6.2 mas/yr pmDE Proper motion in DEC (1)
99-103 F5.2 mas/yr e_pmDE ?=-9.99 Proper motion error in DE (1)
105-109 F5.1 km/s RV ?=-99.9 Radial velocity
111-114 F4.1 km/s e_RV ?=-9.9 Radial velocity error
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Note (1): no value listed in van Leeuwen (2007A&A...474..653V 2007A&A...474..653V, Cat. I/311),
therefore value is set to -9.99
Note (2): Parallax and parallax errors taken from van Leeuwen
(2007A&A...474..653V 2007A&A...474..653V, Cat. I/311)
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Byte-by-byte Description of file: tableb2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- Name BSC Identifier of the star
14- 15 I2 h RAh Right ascension (J2000.0)
17- 18 I2 min RAm Right ascension (J2000.0)
20- 24 F5.2 s RAs Right ascension (J2000.0)
26 A1 --- DE- Declination sign (J2000.0)
27- 28 I2 deg DEd Declination (J2000.0)
30- 31 I2 arcmin DEm Declination (J2000.0)
33- 36 F4.1 arcsec DEs Declination (J2000.0)
38- 42 A5 --- MClass Morphological classification (1)
44 A1 --- Be [x] known Be star ?
46 A1 --- n [x] has a nebulous spectrum ?
48 A1 --- bin [x] known binary ?
50- 56 F7.2 pc d ? Distance determined from the parallax
58- 65 F8.2 pc e_d ? rms uncertainty on Distance
67- 72 F6.2 km/s Vspace ? Space velocity calculated from the radial
velocity, proper motion and distance (2)
74- 78 F5.2 km/s e_Vspace ? Error in space velocity
80- 83 F4.2 arcmin+2 SizeA ? Angular size of the nebulae
85- 90 F6.2 Jy Flux ? Total flux at 22um
92- 98 F7.3 pc+2 Size ? Physical size (3)
100-106 F7.3 pc+2 e_Size ? Error on linear size
108-110 I3 deg alpha ? Misalignment angle between the proper
motion of the star and the bow shock
shape (4)
112-115 F4.1 arcmin R0A ? Angular distance R(0)ang between the
position of the star and the apex of the
bow shock
117-120 F4.2 pc R0 ? Physical distance R(0) between the
position of the star and the apex of the
bow shock
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Note (1): Morphological classification as follows:
bs = bow shock
bsna = not aligned bow shock
cent = centered
unres = unresolved
nc = not classified
Note (2): We determined the total space velocity if the individual uncertainties
in distance, proper motion, and radial velocity measurements were ≤30%.
Note (3): angular size converted to physical size using the distance.
Note (4): It is only given for bow shocks and unaligned bow shocks.
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Acknowledgements:
Julia Bodensteiner, julia.bodensteiner(at)kuleuven.be
(End) J. Bodensteiner [KU Leuven, Belgium], P. Vannier [CDS] 26-Jul-2018