J/A+A/692/A192 C, SB1, SB2 and SB3 southern O stars rotation rate (Blex+, 2024)
The rotation rate of single- and double-lined southern O stars.
Determining what increases the rotation rate in binaries.
Blex S., Haas M., Chini R.
<Astron. Astrophys. 692, A192 (2024)>
=2024A&A...692A.192B 2024A&A...692A.192B (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, spectroscopic ; Stars, O ; Rotational velocities ;
Spectroscopy
Keywords: binaries: spectroscopic - stars: evolution - stars: massive -
stars: rotation -
Abstract:
We determined the projected rotational velocity (vsini) of 238
southern O stars selected from the Galactic O-star Survey. The sample
contains 130 spectroscopic single stars (C), 36 single-lined binaries
(SB1), and 72 SB2 systems (including eight triples). We applied the
Fourier method to high- resolution spectra taken at Cerro Murphy,
Chile, and supplemented by archival spectra. The overall vsini
statistics peaks at slow rotators (40-100km/s) with a tail towards
medium (100-200km/s) and fast rotators (200-400km/s). Binaries, on
average, show increased rotation, which differs for close (Porb<10d)
and wide binaries (10d<Porb<3700d), and for primaries and secondaries.
The spin-up of close binaries is well explained by the superposition
of spin-orbit synchronisation and mass transfer via Roche-lobe
overflow. The increased rotation of wide binaries, however, needs
another explanation. Therefore, we discuss various spin-up mechanisms.
Timescale arguments lead us to favour a scenario where wide O binaries
are spun-up by a combination of cloud or disk fragmentation, which
lays the basis of triple and multiple stars, and the subsequent
merging or swallowing of low-mass by higher-mass stars or proto-stars.
Description:
File tabled1.dat gives the single line sample of C and SB1 stars,
including spectral types, stellar radius and mass, and orbital periods.
File tabled2.dat gives the multiple line sample of SB2 and SB3 systems,
including spectral types of the disentangled components, stellar radius
and mass, previous vsini results, and orbital information.
File tabled3.dat gives the rotation rate of all stars and all lines,
as well as the rotational period.
File tabled4.dat gives a statistics of the spectral lines used.
File refs.dat gives the references for binary types, spectral types,
previous vsini results, and orbital information.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tabled1.dat 95 166 Sample of C+SB1
tabled2.dat 209 72 Sample of SB2+SB3
tabled3.dat 232 318 Rotation rates
tabled4.dat 17 12 Statistics of lines used
refs.dat 70 97 References
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See also:
V/122 : SB9: 9th Catalogue of Spectroscopic Binary Orbits (Pourbaix+ 2005)
III/274 : Galactic O-Star Spectroscopic Survey (GOSSS) (Sota+, 2014)
Byte-by-byte Description of file: tabled1.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Name Star name
15- 21 A7 --- SBtype Binary type [C, SB1] (1)
23- 27 A5 --- SpType Spectral type
29- 41 A13 --- LC Luminosity class
43- 48 A6 --- Refs References, in refs.dat file
50- 52 I3 --- Nspec Total number of spectra
54- 55 I2 --- NBESO Number of BESO spectra
57- 58 I2 --- NFEROS Number of FEROS spectra
60 I1 --- Nother Number of UVES + ELODIE spectra
62- 63 I2 --- n_SBtype ? Notes on SBtype (2)
65- 69 F5.2 Rsun Rstar Calibration stellar radius (3)
71- 75 F5.2 Rsun Mstar Calibration stellar mass (3)
77- 82 F6.1 d Porb ? Orbital period
84- 93 A10 --- r_Porb References for orbital period, in refs.dat file
95 A1 --- n_Porb [1/2]? Notes on orbital period (4)
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Note (1): "C (SB1)" means classified as C by our data but as SB1 by
Holgado et al. (2022A&A...665A.150H 2022A&A...665A.150H). They are used here in the scientific
analysis as SB1.
Note (2): Note on SBtype as follows:
1 = New secure SB1.
2 = HD 046573: Trigueros Paez et al. (2021A&A...655A...4T 2021A&A...655A...4T) found SB1 with
Porb=10.6d and K=11.2km/s. Our data failed to confirm the SB1 and
we assigned "C".
3 = HD 150958: Sota et al. (2014ApJS..211...10S 2014ApJS..211...10S) and Holgado et al.
(2022A&A...665A.150H 2022A&A...665A.150H) reported SB2. We found strong line profile
variations (LPVs) and partly inverse P Cyg profiles.
5 = HD 091651: Sota et al. (2014ApJS..211...10S 2014ApJS..211...10S) reported SB2.
We found SB1 + LPV and eclipses.
6 = HD 152247: Sota et al. (2014ApJS..211...10S 2014ApJS..211...10S) reported SB2, but we did not
see a companion, even with 44 additional UVES spectra between 2007
and 2011.
7 = HD 152314: Sana et al. (2008MNRAS.386..447S 2008MNRAS.386..447S) reported a B1-3 V companion.
Strong LPVs prevented us from identifying lines of a companion.
8 = tau CMa: Sota et al. (2014ApJS..211...10S 2014ApJS..211...10S) reported at least two SB2s,
one spectroscopic binary with P=154d and one eclipsing binary with P=1.2d
but all three companions are faint and not discerned in our spectra.
Based on RV variations we assigned SB1.
9 = HD 053975: Gies et al. 1994 reported SB2 O7.5 V + B2-3 V 3.3mag
difference. The companion is too faint to be detected in our spectra and
its vsini is not known.
10 = HD 152233: Sana et al. (2008MNRAS.386..447S 2008MNRAS.386..447S) reported SB2 O5.5 + O7.5
with a period of 871d. In our spectra, a relatively faint companion was
seen at large dRV but disentangling is not unique and we here adopted
SB1.
11 = HD 152590: Sota et al. (2014ApJS..211...10S 2014ApJS..211...10S) reported SB2. In our 7
spectra, a faint companion is seen at large dRV but disentangling is not
unique.
Note (3): interpolated from Martins et al. (2018A&A...616A.135M 2018A&A...616A.135M) using
SpType and LC.
Note (4): Note on orbital period as follows:
1 = HD 105627: Mahy et al. (2022A&A...664A.159M 2022A&A...664A.159M) determined Porb=4.340874d,
compared to 2.692d reported by Sota et al. (2014ApJS..211...10S 2014ApJS..211...10S).
Both periods yield similar results and conclusions for this paper.
2 = HD 152590: Otero & Claus (2004IBVS.5495....1O 2004IBVS.5495....1O) measured Porb=4.48886d
from eclipses.
From our seven spectra, we find a period of about 3.125d.
Both periods yield similar results and conclusions for this paper.
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Byte-by-byte Description of file: tabled2.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Name Star name
18- 20 A3 --- SBtype [SB2, SB3] Binary type
22- 27 A6 --- SpTypeA Spectral type of primary A (1)
29- 37 A9 --- LCA Luminosity class of A (1)
39- 43 A5 --- SpTypeB Spectral type of secondary B (1)
45- 51 A7 --- LCB Luminosity class of B (1)
53- 58 A6 --- SpTypeC Spectral type of tertiary C (1)
60- 62 A3 --- LCC Luminosity class of C (1)
64- 73 A10 --- r_SpType References for spectral types, in refs.dat file
75- 77 I3 --- Nspec Total number of spectra
79- 80 I2 --- NBESO Number of BESO spectra
82- 84 I3 --- NFEROS Number of FEROS spectra
86 I1 --- Nother Number of UVES + ELODIE spectra
88- 92 A5 --- DT Disentangling type, see Appendix A
94 A1 --- QFA [ABCD] Quality flag of primary (2)
96 A1 --- QFB [ABCDN] Quality flag of secondary (2)
98 A1 --- QFC [ABCD] Quality flag of tertiary (2)
100-104 F5.2 Rsun RstarA Calibration stellar radius of A (3)
106-110 F5.2 Msun MstarA Calibration stellar mass of A (3)
112-116 F5.2 Msun RstarB Calibration stellar radius of B (3)
118-122 F5.2 Msun MstarB Calibration stellar mass of B (3)
124-127 F4.2 Rsun RstarC ? Calibration stellar radius of C (3)
129-133 F5.2 Msun MstarC ? Calibration stellar mass of C (3)
135 I1 --- NoteSB [1/3]? Notes on SBtype, Rstar and Mstar (4)
137 A1 --- l_vsiniA Limit on literature vsini of A
139-141 I3 km/s vsiniA ? Literature vsini of A
143-144 I2 km/s e_vsiniA ? Literature vsini error of A
146 A1 --- l_vsiniB Limit on literature vsini of B
148-150 I3 km/s vsiniB ? Literature vsini of B
152-155 F4.1 km/s e_vsiniB ? Literature vsini error of B
157 A1 --- l_vsiniC Limit on literature vsini of C
159-161 I3 km/s vsiniC ? Literature vsini of C
163-164 I2 km/s e_vsiniC ? Literature vsini error of C
166-174 A9 --- r_vsini References for literature vsini,
in refs.dat file
176-181 F6.1 d Porb ? Literature orbital period
183-186 F4.1 deg i ? Literature orbital inclination
188-191 F4.1 Rsun RlitA ? Literature stellar radius of A
193-196 F4.1 Rsun RlitB ? literature stellar radius of B
198-207 A10 --- r_Porb References for Porb, i, Rlit, in refs.dat file
209 I1 --- Note [1/6]? Notes on literature values (5)
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Note (1): ":" means uncertain, "::" means simply adopted and not determined.
Note (2): disentangling types and quality flags are explained in Appendix A.
QF values (suggested vsini errors) are as follows:
A = very good (10%)
B = good (20%)
C = acceptable (30%)
D = only primary seen (15%)
N = secondary not seen
Note (3): interpolated from Martins (2018A&A...616A.135M 2018A&A...616A.135M) using SpType and LC.
Note (4): Notes on SBtype, Rstar and Mstar as follows:
1 = HD 047129: to derive Rstar and Mstar of B we adopted LC = III.
2 = sigma Ori ABC: Our components A and B correspond to the components
Aa and Ab of Simon-Diaz et al. (2015ApJ...799..169S 2015ApJ...799..169S).
Our spectra did not reveal the tertiary,
a fast rotating early B dwarf, see their Figure 5.
3 = V 961 Cen: In the paper we used for both components A and B
Rlit and Mlit by Penny et al. (2002ApJ...575.1050P 2002ApJ...575.1050P),
instead of Rstar and Mstar.
Note (5): Note as follows:
1 = HD 064315: Lorenzo et al. (2017A&A...606A..54L 2017A&A...606A..54L) reported two binary
systems: a non-eclipsing spectroscopic Aa+Ab with a period of 2.7d,
and an eclipsing fainter Ba+Bb with a period of 1.0d.
The spectroscopic SB2 Aa+Ab dominates the overall appearance.
2 = HD 093205: vsini from FWHM
3 = HD 097166 and HD 123590: orbital inclination computed from Mayer et al.
(2014A&A...565A..86M 2014A&A...565A..86M) using Msin3(i) and Mstar interpolated from
Martins et al. (2018A&A...616A.135M 2018A&A...616A.135M).
4 = HD 100213: vsini is average of several literature values
5 = HD 114886: The period is for components Aa+Ab, which dominate the system,
while component B is faint (Sota et al., 2014ApJS..211...10S 2014ApJS..211...10S).
6 = V 961 Cen: unusually small masses and radii according to Penny et al.
(2002ApJ...575.1050P 2002ApJ...575.1050P)
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Byte-by-byte Description of file: tabled3.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Name Star name
18 A1 --- Comp Component name (1)
20- 22 I3 km/s vsini Best vsini adopted
24- 27 A4 --- n_vsini Origin of best vsini (2)
29- 32 F4.1 d Protsini Rotational period/sini (3)
34- 38 F5.1 km/s vsiniOIII ? vsini of OIII5592
40- 43 F4.1 km/s e_vsiniOIII ? vsini error of OIII5592
45- 46 I2 --- NOIII ?=0 Number of spectra of OIII5592
48- 52 A5 km/s vsiniHeI ? Average vsini of HeI lines
54- 57 F4.1 km/s e_vsiniHeI ? vsini error of HeI lines
59 I1 --- NHeI ?=0 Number of HeI lines used
61- 63 I3 --- NtotHeI ?=0 Total number of HeI spectra
65- 69 F5.1 km/s vsiniHeII ? average vsini of HeII lines
71- 74 F4.1 km/s e_vsiniHeII ? vsini error of HeII lines
76 I1 --- NHeII ?=0 Number of HeII lines used
78- 79 I2 --- NtotHeII ?=0 Total number of HeII spectra
81- 85 F5.1 km/s vsiniHeI4026 ? vsini of HeI4026
87- 90 F4.1 km/s e_vsiniHeI4026 ? vsini error of HeI4026
92- 93 I2 --- NHeI4026 ?=0 Number of HeI4026 spectra used
95- 99 F5.1 km/s vsiniHeI4387 ? vsini of HeI4387
101-104 F4.1 km/s e_vsiniHeI4387 ? vsini error of HeI4387
106-107 I2 --- NHeI4387 ?=0 Number of HeI4387 spectra used
109-113 F5.1 km/s vsiniHeI4471 ? vsini of HeI4471
115-118 F4.1 km/s e_vsiniHeI4471 ? vsini error of HeI4471
120-121 I2 --- NHeI4471 ?=0 Number of HeI4471 spectra used
123-127 F5.1 km/s vsiniHeI4922 ? vsini of HeI4922
129-132 F4.1 km/s e_vsiniHeI4922 ? vsini error of HeI4922
134-135 I2 --- NHeI4922 ?=0 Number of HeI4922 spectra used
137-141 F5.1 km/s vsiniHeI5876 ? vsini of HeI5876
143-146 F4.1 km/s e_vsiniHeI5876 ? vsini error of HeI5876
148-149 I2 --- NHeI5876 ?=0 Number of HeI5876 spectra used
151-155 F5.1 km/s vsiniHeI6678 ? vsini of HeI6678
157-160 F4.1 km/s e_vsiniHeI6678 ? vsini error of HeI6678
162-163 I2 --- NHeI6678 ?=0 Number of HeI6678 spectra used
165-169 F5.1 km/s vsiniHeI7065 ? vsini of HeI7065
171-174 F4.1 km/s e_vsiniHeI7065 ? vsini error of HeI7065
176-177 I2 --- NHeI7065 ?=0 Number of HeI7065 spectra used
179-183 F5.1 km/s vsiniHeII4200 ? vsini of HeII4200
185-188 F4.1 km/s e_vsiniHeII4200 ? vsini error of HeII4200
190 I1 --- NHeII4200 ?=0 Number of HeII4200 spectra used
192-196 F5.1 km/s vsiniHeII4541 ? vsini of HeII4541
198-201 F4.1 km/s e_vsiniHeII4541 ? vsini error of HeII4541
203-204 I2 --- NHeII4541 ?=0 Number of HeII4541 spectra used
206-210 F5.1 km/s vsiniHeII4686 ? vsini of HeII4686
212-215 F4.1 km/s e_vsiniHeII4686 ? vsini error of HeII4686
217-218 I2 --- NHeII4686 ?=0 Number of HeII4686 spectra used
220-224 F5.1 km/s vsiniHeII5411 ? vsini of HeII5411
226-229 F4.1 km/s e_vsiniHeII5411 ? vsini error of HeII5411
231-232 I2 --- NHeII5411 ?=0 Number of HeII5411 spectra used
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Note (1): blank for single line stars. [A,B,C] for primary, secondary and
tertiary of multiple line stars, respectively.
Note (2): OIII, HeI (see Section 4.1) or Lit (= from tabled1 and tabled2).
Note (3): rotational period/sin(i)=radius/vsini, where stellar radius
is taken from from tabled1 and tabled2, respectively.
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Byte-by-byte Description of file: tabled4.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- LineName Line name
11- 13 I3 --- Nsingle Number of C+SB1 stars using the line
15- 17 I3 --- Nmulti Number of stars in SB2+SB3 using the line
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ref Reference number
4- 26 A23 --- Aut Author's name
29- 47 A19 --- BibCode BibCode
49- 70 A22 --- Com Comments
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Acknowledgements:
Susanne Blex, susanne.blex(at)rub.de
(End) Patricia Vannier [CDS] 11-Nov-2024