J/A+A/384/491 Fast-rotating nearby solar-type stars. I. (Cutispoto+, 2002-03)
Fast-rotating nearby solar-type stars.
I. Spectral classification, vsini, Li abundances and X-ray luminosities
Cutispoto G., Pastori L., Pasquini L., de Medeiros J.R., Tagliaferri G.,
Andersen J.
<Astron. Astrophys. 384, 491 (2002)>
=2002A&A...384..491C 2002A&A...384..491C
II. Li abundances, vsini and X-ray luminosities relationships.
Cutispoto G., Tagliaferri G., de Medeiros J.R., Pastori L., Pasquini L.,
Andersen J.
<Astron. Astrophys. 397, 987 (2003)>
=2003A&A...397..987C 2003A&A...397..987C
ADC_Keywords: Stars, nearby ; Stars, G-type ; Photometry, UBVRI ; Abundances ;
Radial velocities ; Rotational velocities ; Equivalent widths
Keywords: stars: abundances - stars: activity - stars: fundamental parameters -
stars: variables: general - X-rays: stars
Abstract:
We present the results of high-resolution spectroscopic and
high-precision photometric observations on a sample of 129 late-F and
G-type nearby stars selected on the basis of their large rotational
velocity. Using also data from the Hipparcos satellite, CORAVEL and
from the ROSAT satellite database, we infer spectral types, compute
radial velocities, vsini, Li abundances and X-ray luminosities and
investigate the single or binary nature of the sample stars. Such a
careful analysis of our sample shows a large fraction of binaries
(∼62%) and of young single disk stars. In particular, at least 9 stars
can be considered bona-fide PMS or ZAMS objects, and 30 stars are
identified as SBs for the first time. Information on the presence of
Ca II K emission and on optical variability is given for some of the
stars of the sample.
The photometry has been obtained at the European Southern Observatory
(ESO-La silla, Chile) during several observing runs (19/11-03/12 1993,
24/11-04/12 1994, 15-28/01/1995 and 1-12/10/1995), by using the 50cm
ESO telescope.
The figures were published in paper II.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 102 173 Summary of stellar data (Paper I)
table3.dat 102 25 Summary of stellar data for stars excluded from
the analysis (Paper I)
table4.dat 37 90 UBV(RI)c photometry from La Silla (Paper I)
table5.dat 36 304 Radial velocity determinations (Paper I)
notes.dat 80 403 Individual notes (Paper I)
figure1.ps 102 7017 *The B-V vs. MV diagram , all sample stars
figure2.ps 102 2584 *A(Li) vs. logTeff, single stars
figure3.ps 102 1898 *A(Li) vs. logTeff, close binaries
figure4.ps 102 2054 *A(Li) vs. vsini, single and binary
figure5.ps 102 2141 *L(X) vs. vsini, RASS single and binary
figure6.ps 102 1240 *L(X) vs. A(Li), single stars
figure7.ps 102 586 *L(X) vs. A(Li), binary sample
figure8.ps 102 4849 *log(L/L☉) vs. logTeff, PMS and evolved stars
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Note on figure1.ps:
The B-V vs. MV diagram for the stars in our sample. Single stars and
primary and secondary components of VBs and of SBs are identified by
different symbols. The continuous line and the long-dashed line
outline the main sequence and giant regions, respectively, from
Hipparcos data (Houk et al., 1997, in Proc. Hipparcos Venice 97 Symp.,
ESA SP-402, 279); the short-dashed lines indicate the limits of the
dispersion of main sequence stars from Hipparcos data. Panel (a) shows
the complete sample; panel (b) shows the stars we believe to be very
young
Note on figure2.ps:
A(Li) vs. logTeff for single stars and single VB components. Symbols
as in Fig. 1. Panel a: Stars on the main sequence; the solid and
dashed curves are the fiducial A(Li) vs. logTeff curves for the
Pleiades (top envelope) and the Hyades clusters, respectively (adapted
from Deliyannis, 2000, in Stellar Clusters and Associations, ASP Conf.
Ser., 198, 235). Panel b: stars above the main sequence; the area
inside the quadrangle is the region populated by subgiants, giants and
supergiants (adapted from Mallik, 1999A&A...352..495M 1999A&A...352..495M). The Sun's
position is shown in both panels.
Note on figure3.ps:
A(Li) vs. logTeff for the close binaries. Symbols as in Fig. 1.
Panel a: MS stars; the solid and dashed curves are the fiducial A(li) vs.
logTeff curves for the Pleiades (top envelope) and Hyades,
respectively (adapted from Deliyannis 2000, ASP Conf. Ser., 198, 235).
Panel b: stars above the MS; the area inside the quadrangle is the
region populated by subgiants, giants and supergiants (adapted from
Mallik, 1999A&A...352..495M 1999A&A...352..495M). The Sun's position is shown in both
panels.
Note on figure4.ps:
A(Li) vs. vsini for single (a) and binary stars (b). Note that while
all single stars with vsini>18km/s have A(Li)≥2.0, there are binaries
with vsini∼30km/s for which only an upper limit to A(Li) was obtained.
In our sample of fast rotators, single stars have, on average, higher
A(Li) values than binary stars.
Note on figure5.ps:
L(X) vs. vsini for the single (a) and binary (b) stars in our sample
detected in the RASS. As expected, L(X) correlates with vsini,
although with a large scatter, and all fast rotators are also very
active in X-rays (with the exception of a few stars that are not
detected, see text).
Note on figure6.ps:
L(X) vs. A(Li) for single stars. Symbols are as in Fig. 1.
Panel a: stars on the main sequence; Panel b: stars above the main
sequence. L(X) is clearly correlated with A(Li). The correlation is
particularly prominent for non-MS stars (panel b), although the latter
sample is rather small and the correlation is dominated by the two PMS
candidates.
Note on figure7.ps:
L(X) vs. A(Li) for the binary sample. Symbols as in Fig. 1.
Panel a: MS stars; Panel b: stars above the main sequence.
No correlation is apparent
Note on figure8.ps:
log(L/L☉) vs. logTeff diagram for the PMS and evolved stars of
our sample. Symbols are as in Fig. 1. Panel (a) shows the stars
believed to be PMS objects as well as evolutionary tracks (continuous
lines) and isochrones (dotted lines) for PMS stars (adapted from
D'Antona & Mazzitelli, 1997MmSAI..68..807D 1997MmSAI..68..807D). Panel (b) shows the stars
found to lie above the upper limit of the Hipparcos MS (see Fig. 1) as
well as evolutionary tracks (continuous lines) and the 100 Myr
isochrone (dotted line) for evolved stars (adapted from Ventura et
al., 1998A&A...334..953V 1998A&A...334..953V).
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See also:
J/A+AS/138/87 : UBVRI photometry of EUV stellar sources (Cutispoto+ 1999)
J/A+A/384/491 : Fast-rotating nearby solar-type stars. II. (Cutispoto+, 2003)
Byte-by-byte Description of file: table1.dat table3.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- --- [HD]
4- 9 I6 --- HD Program star HD number
10- 11 A2 --- m_HD Multiplicty index on HD
13- 17 F5.2 mag Vmag ? V magnitude
19- 21 A3 --- Bin Binarity flag (VB or SB)
23- 37 A15 --- SpType Inferred spectral type (1)
39- 44 F6.1 pc Dist ? Trigonometric or photometric distance
45 A1 --- u_Dist Uncertainty flag on Dist
47- 51 F5.2 mag VMAG ? Absolute V magnitude
52 A1 --- u_VMAG Uncertainty flag on VMAG (1)
54- 56 I3 km/s vsini ? vsini from our spectra
57 A1 --- u_vsini Uncertainty flag on vsini (1)
58 A1 --- n_vsini [b] b: blended (2)
59 A1 --- --- [+] If two vsini for binaries
60- 61 I2 km/s vsini2 ? Second vsini value from our spectra
for binaries
62 A1 --- u_vsini2 [:?] Uncertainty flag on vsini2, or
? for unknown (1)
64- 66 I3 km/s vsiniCO ? vsini from the CORAVEL database
67 A1 --- u_vsiniCO Uncertainty flag on vsiniCO (1)
68 A1 --- n_vsiniCO [b] b: blended (2)
69 A1 --- --- [+] If two vsini for binaries
70- 71 I2 km/s vsini2CO ? Second vsini value from the CORAVEL database
72 A1 --- u_vsini2CO [:?] Uncertainty flag on vsini2CO, or
? for unknown (1)
74 A1 --- l_EWLi Limit flag on EWLi
75- 77 I3 0.1pm EWLi ? Li line equivalent width in milli-Angstrom
78 A1 --- --- [+] If two equivalent width for binaries
79 A1 --- l_EWLi2 Limit flag on EWLi2
80- 82 I3 0.1pm EWLi2 ? Second Li line equivalent width for binaries
84 A1 --- l_ALi Limit flag on ALi
85- 88 F4.1 --- ALi ? Li abundance (H abundance = 12)
89 A1 --- n_ALi [*] *: Abundance computed in LTE
90 A1 --- --- [+] If two abundances for binaries
91 A1 --- l_ALi2 Limit flag on ALi2
92- 94 F3.1 --- ALi2 ? Second Li abundance for binaries
(H abundance = 12)
95 A1 --- n_ALi2 [*] *: Abundance computed in LTE
97-100 F4.1 [10-7W] LX ? log of the X-ray luminosity in the
0.2-2.6keV band
102 A1 --- Note [*] *: Note explained in notes.dat file
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Note (1): Errors uncertainties:
SpType : ":" denotes errors up to several spectral subclasses
VMAG: ":" denotes values computed from the photometric parallax
vsini: errors are of the order of ±1km/s,
the symbol ":" denotes errors up to ±3km/s;
Note (2): The symbol "b" denotes blended values for those VB or SB2 or SB3
systems for which it was not possible to separate the contribution
of the individual components
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- --- [HD]
4- 9 I6 --- HD Program star HD number
10- 11 A2 --- m_HD Multiplicty index on HD
13- 16 F4.2 mag Vmag V magnitude
18- 21 F4.2 mag U-B U-B colour index
22 A1 --- n_U-B Uncertainty flag on U-B
24- 27 F4.2 mag B-V B-V colour index
29- 32 F4.2 mag V-R V-R Cousins colour index
34- 37 F4.2 mag V-I V-I Cousins colour index
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- --- [HD]
4- 9 I6 --- HD HD number
10- 11 A2 --- m_HD Multiplicity index on HD (1)
13- 22 A10 "DD/MM/YYYY" Date Observation date
24- 28 F5.1 km/s RV Radial velocity
30- 33 F4.1 km/s e_RV rms uncertainty on RV
35- 36 A2 --- Line [Ca Li] Spectral region from which the RV
was computed (2)
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Note (1): The components of VBs and the components of SBs are indicated with
capitals and lower case letters, respectively.
Note (2): Spectral regions:
Ca: Ca IIK, centered at 3938.5Å
Li: Li I, centered at 6705.5Å
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Byte-by-byte Description of file: notes.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- HD HD number
8- 80 A73 --- Note Text of the note
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History: On 30-Sep-2003, In table4, last colour index corrected into V-I.
Acknowledgements: Giuseppe Cutispoto
(End) Patricia Bauer [CDS] 11-Mar-2002