J/A+A/675/A180 Rotation of wide binaries (Gruner+, 2023)
Wide binaries demonstrate the consistency of rotational evolution between open
cluster and field stars.
Gruner D., Barnes S.A., Janes K.A.
<Astron. Astrophys. 675, A180 (2023)>
=2023A&A...675A.180G 2023A&A...675A.180G (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Stars, late-type ; Stars, variable ;
Stars, nearby ; Stars, ages ; Photometry ; Optical
Keywords: binaries: general - stars: late-type - stars: rotation - starspots
Abstract:
Gyrochronology allows the derivation of ages of late-type main
sequence stars from their rotation periods and a mass proxy such as
color. It has been explored in open clusters, but a connection to
field stars has yet to be established successfully. We explore the
rotation rates of wide binaries, representing enlightening
intermediaries between clusters and field stars, and their overlap
with those of open cluster stars. We investigate a recently created
catalog of wide binaries, match them to observations by the Kepler
mission (and its K2 extension), validate or rederive their rotation
periods, identify 283 systems where both stars are on the main
sequence and have vetted rotation periods, and compare them with open
cluster data. We find that the vast majority of these wide binaries
(236) line up directly along the curvilinear ribs defined by open
clusters in color-period diagrams or along the equivalent interstitial
gaps between successive open clusters. The parallelism in shape is
remarkable. 12 additional systems are clearly rotationally older. The
deviant systems, a minority, are mostly demonstrably hierarchical.
Furthermore, the position in the color-magnitude diagram of the
evolved component in the additional wide binary systems containing one
is consistent with the main sequence component's rotational age.
Description:
We present a compilation of wide binaries from El-Badry et al.
(2021MNRAS.506.2269E 2021MNRAS.506.2269E) crossmatched with Kepler and K2 observations.
The wide binaries are subsequently investigated for consistency of
rotation of the individual components in comparison to stellar open
clusters.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablec1.dat 335 744 Compilation of wide binaries
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See also:
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
V/133 : Kepler Input Catalog (KIC) (Kepler Mission Team, 2009)
IV/34 : K2 Ecliptic Plane Input Catalog (EPIC) (Huber+, 2017)
I/355 : Gaia DR3 Part 1 (Gaia Collaboration, 2022)
J/ApJS/211/24 : Rotation periods of Kepler MS stars (McQuillan+, 2014)
J/A+A/635/A43 : Stellar rotation periods from K2 Campaigns 0-18
(Reinhold+, 2020)
Byte-by-byte Description of file: tablec1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Binary Sample binary
5 I1 --- Agegroup [1/7] Assigned age group (1)
7 A1 --- Class [CEFSW] Assign binary class (2)
9- 20 A12 --- Problem Note on a contradicting WB system (3)
22- 40 I19 --- GaiaDR3 Gaia DR3 identifier
42- 58 A17 --- 2MASS 2MASS identifier
60- 68 I9 --- EPIC ? EPIC identifier
70- 77 I8 --- KIC ? KIC identifier
79- 89 A11 --- Notes Notes on the individual stars (4)
91- 95 F5.2 d Prot ? Rotation period
97-101 F5.2 d e_Prot ? Error on rotation period
103-109 F7.4 mag Gmag Gaia DR3 Gmag
111-116 F6.4 mag e_Gmag Error on Gaia DR3 Gmag
118-124 F7.4 mag BPmag Gaia DR3 BPmag
126-131 F6.4 mag e_BPmag Error on Gaia DR3 BPmag
133-139 F7.4 mag RPmag Gaia DR3 RPmag
141-146 F6.4 mag e_RPmag Error on Gaia DR3 RPmag
148-154 F7.4 mag BP-RP Gaia DR3 BP-RP color
156-161 F6.4 mag e_BP-RP Error on Gaia DR3 BP-RP color
163-169 F7.4 mag G-RP Gaia DR3 G-RP color
171-176 F6.4 mag e_G-RP Error on Gaia DR3 G-RP color
178-187 F10.6 deg RAdeg Gaia DR3 Right Ascension (ICRS)
at Ep=2016.0
189-198 F10.6 deg DEdeg Gaia DR3 Declination (ICRS) at Ep=2016.0
200-207 F8.3 mas/yr pmRA Gaia DR3 proper motion in RA
209-213 F5.3 mas/yr e_pmRA Error on Gaia DR3 proper motion in RA
215-222 F8.3 mas/yr pmDE Gaia DR3 proper motion in DE
224-228 F5.3 mas/yr e_pmDE Error on Gaia DR3 proper motion in DE
230-236 F7.4 mas plx Gaia DR3 parallax
238-243 F6.4 mas e_plx Error on Gaia DR3 parallax
245-250 F6.2 km/s RV ? Gaia DR3 radial velocity
252-256 F5.2 km/s e_RV ? Error on Gaia DR3 radial velocity
258-262 F5.2 d ProtMQ14 ? Rotation period in MQ14 [d]
264-267 F4.2 d e_ProtMQ14 ? Error on Rotation period in MQ14
269-273 F5.2 d ProtRH20 ? Rotation period in RH20
275-279 F5.2 d e_ProtRH20 ? Error on Rotation period in RH20
281-286 F6.3 --- [Fe/H]gaia3 ? Iron abundance in Gaia DR3
288-292 F5.3 --- e_[Fe/H]gaia3 ? Error on Iron abundance in Gaia DR3
294-299 F6.3 --- [M/H]TIC ? Metallicity in TIC
301-305 F5.3 --- e_[M/H]TIC ? Error on Metallicity in TIC
307-313 F7.2 Myr AgeBPH23 ? Age calculated with gyrointerp
315-321 F7.2 Myr e_AgeBPH23 ? Lower error on gyrointerp age
323-335 F13.9 Myr E_AgeBPH23 ? Upper error on gyrointerp age
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Note (1): Age grouping according to Sect. 2.3 of the paper as follows:
1 = 0 ≤ t < 500Myr,
2 = 500Myr ≤ t ≤ 1Gyr
3 = 1Gyr < t < 2.5Gyr
4 = 2.5Gyr ≤ t ≤ 2.7Gyr
5 = 2.7Gyr < t < 4Gyr
6 = t = 4Gyr
7 = t > 4Gyr
Note (2): Binary system classification according to Sect. 3 of the paper
as follows:
S = MS+MS binary, both on slow rotator sequence
F = MS+MS binary, at least one star is a fast rotator
C = MS+MS binary, system contradicts open cluster behavior
E = MS+(sub)giant system
W = MS+WD system
Note (3): If system is class C, indication for disagreement as follows:
hierarchical = one star is a double
unknown = no indication
Note (4): Additional note on individual stars. Indicates whether a star is a
(sub)giant or a white dwarf. "Double" means a star is a binary itself.
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Acknowledgements:
David Gruner, dgruner(at)aip.de
(End) Patricia Vannier [CDS] 23-May-2023