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J/AJ/105/2299     Li abundance of solar-type stars. II.       (Soderblom+, 1993)

The evolution of the lithium abundances of solar-type stars. II. The Ursa Major group SODERBLOM D.R., PILACHOWSKI C.A., FEDELE S.B., JONES B.F. <Astron. J. 105, 2299 (1993)> =1993AJ....105.2299S (SIMBAD/NED Reference)
ADC_Keywords: Stars, G-type; Stars, dwarfs; Combined data; Abundances Abstract: We draw upon a recent study of the membership of the Ursa Major Group (UMaG) to examine lithium among 0.3 Gyr old solar-type stars. For most G and K dwarfs, Li confirms the conclusions about membership in UMaG reached on the basis of kinematics and chromospheric activity. G and K dwarfs in UMaG have less Li than comparable stars in the Pleiades. This indicates that G and K dwarfs undergo Li depletion while they are on the main sequence, in addition to any pre-main-sequence depletion they may have experienced. Moreover, the Li abundances of the Pleiades K dwarfs cannot be attributed to main-sequence depletion alone, demonstrating that pre-main-sequence depletion of Li also takes place. The Sun's Li abundance implies that the main-sequence mechanism becomes less effective with age, otherwise the Sun would have even less Li than it does. The hottest stars in the UMaG (T(eff) ≳ 6800K) have Li abundances like those of hot stars in the Pleiades and Hyades and in T Tauris, and the two genuine UMaG members with temperatures near Boesgaard's Li chasm have Li abundances consistent with that chasm developing fully by 0.3 Gyr for stars with UMaG's metallicity ([Fe/H] = -0.08 ± 0.09). We see differences in the abundance of Li between UMaG members of the same spectral types, indicating that a real spread in the lithium abundance exists within this group. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1 88 46 Lithium abundances of UMaG solar-type stars table2 58 36 *Colors and temperatures of UMaG candidates
Note on table2: The photometry has been taken from Nicolet (1978), Hauck & Mermilliod (1980) and Mendoza (1967). Note that no corrections for reddening have been made for these nearby (d ≤ 25 pc) stars.
Byte-by-byte Description of file: table1
Bytes Format Units Label Explanations
1 A1 --- Member [abc] Membership probability as: a: Probable member b: Possible member c: Probable non-member 2- 7 I6 --- HD Henry Draper number 8- 9 A2 --- m_HD Multiplicity index on HD number 11- 14 I4 --- HR []? Harvard Revised (Brigth Star) number 15- 16 A2 --- m_HR Multiplicity index on HR number 18- 28 A11 --- Name Other name 30- 33 A4 --- Sp Spectral type 36- 39 F4.2 mag B-V (B-V) color 40 A1 --- u_B-V Uncertainty flag on B-V 41- 45 I5 K Teff Effective temperature (average of the temperatures listed in table2) 46 A1 --- u_Teff Uncertainty flag on B-V 47 A1 --- l_W(Li)L limit flag on W(Li)L 48- 49 I2 0.1pm W(Li)L []? Measured equivalent width for Li 6708 A feature from Lick Hamilton spectrograph 50 A1 --- u_W(Li)L uncertainty flag on W(Li)L 51 A1 --- l_W(Li)K limit flag on W(Li)K 52- 53 I2 0.1pm W(Li)K []? Measured equivalent width for Li 6708 A feature from Kitt Peak 54 A1 --- u_W(Li)K uncertainty flag on W(Li)K 56 A1 --- l_W(Li)B limit flag on W(Li)B 57- 60 F4.1 0.1pm W(Li)B []? Measured equivalent width for Li 6708 A feature from Boesgaard et al. (1988) 62- 63 I2 0.1pm W(Li)R []? Measured equivalent width for Li 6708 A feature from Lick Reticon 66 A1 --- l_W(Li)E limit flag on W(Li)E 67- 68 I2 0.1pm W(Li)E []? Measured equivalent width for Li 6708 A feature from ESO 70 A1 --- l_W(Li)I limit flag on W(Li)I 71 I1 0.1pm W(Li)I []? Equivalent width for Li 6708 A feature (origin not precised) 77 A1 --- l_<W(Li)> limit flag on <W(Li)> 78- 79 I2 0.1pm <W(Li)> Adopted mean equivalent width 82 A1 --- l_log(N(Li)) limit flag on log(N(Li)) 83- 87 F5.2 --- log(N(Li)) Log of the lithium abundance, log(N(Li)), where log N(H) = 12 88 A1 --- u_log(N(Li)) Uncertainty flag on B-V
Byte-by-byte Description of file: table2
Bytes Format Units Label Explanations
1- 6 I6 --- HD Henry Draper number 7- 8 A2 --- m_HD Multiplicity index on HD number 9- 14 F6.2 mag B-V (B-V) color 15- 20 I6 K Teff(B-V) Effective temperature inferred from (B-V) 21- 27 F7.3 mag b-y []? Stromgren color index (b-y) 28- 33 I6 K Teff(b-y) []? Effective temperature inferred from color index (b-y) 34- 40 F7.3 mag Beta []? Stromgren beta index 41- 46 I6 K Teff(Beta) []? Effective temperature inferred from beta index 47- 52 F6.2 mag V-I []? Johnson color index (V-I) 53- 58 I6 K Teff(V-I) []? Effective temperature inferred from color index (V-I)
References: Hauck B. & Mermilliod M. 1980, A&AS, 40, 1 Mendoza E.E. 1967, Bol. Obs. Tonantzintla y Tacubaya, 4, 149 Nicolet B. 1978, A&AS, 34, 1 Origin: AAS CD-ROM series, Volume 1, 1993
(End) Patricia Bauer [CDS] 06-Jul-1994
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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