J/MNRAS/487/3162 Debris disc stars metallicity & Li properties (Chavero+, 2019)
Emerging trends in metallicity and lithium properties of debris disc stars.
Chavero C., de la Reza R., Ghezzi L., Llorente de Andres F., Pereira C.B.,
Giuppone C., Pinzon G.
<Mon. Not. R. Astron. Soc. 487, 3162-3177 (2019)>
=2019MNRAS.487.3162C 2019MNRAS.487.3162C (SIMBAD/NED BibCode)
ADC_Keywords: Stars, dwarfs ; Infrared sources ; Abundances, [Fe/H]
Keywords: planets and satellites: formation - stars: abundances -
circumstellar matter - planetary systems - stars: solar-type
Abstract:
Dwarf stars with debris discs and planets appear to be excellent
laboratories to study the core accretion theory of planets formation.
These systems are however, insufficiently studied. In this paper we
present the main metallicity and lithium abundance properties of these
stars together with stars with only debris discs and stars with only
planets. Stars without detected planets nor discs are also considered.
The analysed sample is formed by main-sequence FGK field single stars.
Apart from the basic stellar parameters, we include the use of dusty
discs masses. The main results show for the first time that the dust
mass of debris disc stars with planets correlate with metallicity. We
confirm that these disc dust masses are related to their central
stellar masses.
Separately, the masses of stars and those of planets also correlate
with metallicity. We conclude that two conditions are necessary to
form giant planets: to have a sufficient metallicity and also a
sufficient protoplanetary mass of gas and dust. The debris discs
masses of stars without giant planets do not correlate with
metallicity, because they do not fulfil these two conditions.
Concerning lithium, by adopting a stellar model for lithium depletion
based on a strong interaction between the star and a protoplanetary
disc, we found that in agreement with the model predictions,
observations indicate that the main lithium depletion occurs during
this initial protoplanetary evolution stage. We show that the
ultimately lithium depletion is independent of the presence or absence
of planets and appears to be only age dependent.
Description:
File table1 lists the whole collection of the stars related to this
work (C, CP, D and DDP sample) with their stellar properties and
references of the IR data in Note 2. The stellar ages and masses were
derived using L. Girardi on-line code PARAM 1.3
(http://stev.oapd.inaf.it/cgi-bin/param), see also Da Silva et al.
(2006A&A...458..609D 2006A&A...458..609D). This table1 also provide lithium abundances and
the dust mass (LOG).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 102 140 Parameters of the stellar sample
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See also:
J/A+A/541/A40 : Metallicity of solar-type stars (Maldonado+, 2012)
J/A+A/579/A20 : Circumstellar debris discs (Maldonado+, 2015)
J/A+A/593/A51 : Debris discs around nearby FGK stars (Montesinos+, 2016)
J/MNRAS/449/3160 : Stellar multiplicity and debris discs (Rodriguez+, 2015)
J/A+A/614/A3 : 6 cold-gas-bearing debris-disc stars spectra
(Rebollido+, 2018)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- HD HD number
7 A1 --- m_HD Multiplicity index on HD
9- 11 A3 --- Group Group (1)
13- 17 A5 --- SpType Hipparcos MK spectral-type
19- 22 F4.2 Msun M* Stellar mass
24- 27 F4.2 Msun e_M* Uncertainty on the stellar mass
29- 34 F6.3 Gyr Age Stellar Age
36- 40 F5.2 Gyr e_Age ? Uncertainty on stellar Age
42 A1 --- RefIR References of Infrared data (2)
44- 47 I4 K Teff Effective Temperature
49- 53 F5.2 [Sun] [Fe/H] Metallicity
55- 58 F4.2 [Sun] e_[Fe/H] Uncertainty on metallicity
60- 63 F4.2 [cm/s2] logg ? Surface gravity
65 A1 --- l_vsini ? Upper limit flag on rotational velocity
66- 69 F4.1 km/s vsini ? Rotational Velocity
71 A1 --- l_A(Li) ? Upper limit flag on A(Li)
72- 76 F5.2 [-] A(Li) ? Lithium Abundance
78- 81 F4.2 [-] e_A(Li) ? Formal Uncertainty on A(Li)
83- 87 F5.2 [0.012Mgeo] Log(Md) ? Log dust mass
(Md is in lunar mass units)
89 I1 --- r_Log(Md) ? References of Md determination (3)
91-102 A12 --- Refs References of stellar parameters
and A(li) (4)
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Note (1): Taking into account IR data the groups are as follows:
C = Stars without known debris discs or planet
CP = Stars with only planets
DD = Stars with only debris discs
DDP = Stars with known debris disc and planet
Note (2): References of Infrared data suing to divide de four groups defined in
this group as follows:
a = Trilling et al. (2008ApJ...674.1086T 2008ApJ...674.1086T)
b = Kospal et al. (2009ApJ...700L..73K 2009ApJ...700L..73K)
c = Plavchan et al. (2009ApJ...698.1068P 2009ApJ...698.1068P)
d = Bryden et al. (2006ApJ...636.1098B 2006ApJ...636.1098B)
e = Bryden et al. (2009ApJ...705.1226B 2009ApJ...705.1226B)
f = Chen et al. (2014ApJS..211...25C 2014ApJS..211...25C)
g = Maldonado et al. (2012A&A...541A..40M 2012A&A...541A..40M)
h = Beichman et al. (2006ApJ...652.1674B 2006ApJ...652.1674B)
i = Koerner et al. (2010ApJ...710L..26K 2010ApJ...710L..26K)
j = Greaves et al. (2004MNRAS.351L..54G 2004MNRAS.351L..54G)
k = Hillenbrand et al. (2008ApJ...677..630H 2008ApJ...677..630H)
l = Rhee et al. (2007ApJ...660.1556R 2007ApJ...660.1556R)
m = Kalas et al. (2006ApJ...637L..57K 2006ApJ...637L..57K)
n = Carpenter et al. (2008ApJS..179..423C 2008ApJS..179..423C)
o = Eiroa et al. (2013A&A...555A..11E 2013A&A...555A..11E)
Note (3): References of Md determination as follows:
1 = Chen et al., (2014ApJS..211...25C 2014ApJS..211...25C
2 = Derived in this work
Note (4): References of stellar parameters and A(li) as follows:
TW = This work
G10 = Ghezzi et al. (2010ApJ...724..154G 2010ApJ...724..154G)
GO10 = Gonzalez et al. (2010MNRAS.403.1368G 2010MNRAS.403.1368G)
S08 = Sousa et al. (2008A&A...487..373S 2008A&A...487..373S)
L06 = Luck & Heiter et al. (2006AJ....131.3069L 2006AJ....131.3069L)
R12 = Ramirez et al. (2012ApJ...756...46R 2012ApJ...756...46R)
M12 = Maldonado et al. (2012A&A...541A..40M 2012A&A...541A..40M)
S04 = Santos et al. (2004A&A...415.1153S 2004A&A...415.1153S)
DM14 = Delgado-Mena et al. (2014A&A...562A..92D 2014A&A...562A..92D)
V05 = Valenti et al. (2005ApJS..159..141V 2005ApJS..159..141V)
B91 = Boesgaard et al. (1991ApJ...370L..95B 1991ApJ...370L..95B)
C11 = Casagrande et al. (2011A&A...530A.138C 2011A&A...530A.138C)
E12 = Ertel et al. (2012A&A...541A.148E 2012A&A...541A.148E)
G16 = Gaspar et al. (2013ApJ...768...25G 2013ApJ...768...25G)
S06 = Sousa et al. (2006A&A...458..873S 2006A&A...458..873S)
L17 = Luck et al. (2017AJ....153...21L 2017AJ....153...21L)
A18 = Aguilera et al. (2018A&A...614A..55A 2018A&A...614A..55A)
B15 = Bell et al. (2015MNRAS.454..593B 2015MNRAS.454..593B)
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Acknowledgements:
Carolina Chavero, tali(at)mail.oac.uncor.edu
(End) Carolina Chavero [OAC-UNC-CONICET], Patricia Vannier [CDS] 30-May-2019