J/AJ/149/59 Abundances of ρ Pup (Yushchenko+, 2015)
The chemical composition of ρ Puppis and the signs of accretion in the
atmospheres of B-F-Type stars.
Yushchenko A.V., Gopka V.F., Kang Y.-W., Kim C., Lee B.-C.,
Yushchenko V.A., Dorokhova T.N., Doikov D.N., Pikhitsa P.V., Hong K.,
Kim S., Lee J.-W., Rittipruk P.
<Astron. J., 149, 59 (2015)>
=2015AJ....149...59Y 2015AJ....149...59Y
ADC_Keywords: Stars, variable ; Abundances ; Equivalent widths
Keywords: accretion, accretion disks - circumstellar matter -
stars: abundances - stars: chemically peculiar -
stars: individual: * rho Pup - stars: rotation
Abstract:
We investigated the chemical composition of ρ Pup using
high-resolution spectral observations taken from the Very Large
Telescope and the IUE archives and also spectra obtained at the 1.8m
telescope of the Bohyunsan observatory in Korea. The abundances of 56
chemical elements and the upper limits of Li and Be abundances were
determined. The abundance pattern of ρ Pup was found to be similar
to that of Am-type stars. The possibility of the influence of the
accretion of interstellar gas and dust on the abundance patterns of
B--F-type stars is discussed. The plots of the relative abundances of
chemical elements in the atmospheres of ρ Pup and δ Sct
versus the second ionization potentials of these elements show the
correlations. The discontinuities at 13.6 and 24.6eV--the ionization
potentials of hydrogen and helium, respectively, are also exhibited in
these plots. These discontinuities can be explained by interaction of
the atoms of interstellar gas, mainly hydrogen and helium atoms, with
the atoms of stellar photospheres (so-called charge-exchange
reactions). Note that only the jumps near 13.6 and 24.6eV were pointed
out in previous investigations of relative abundances versus the
second ionization potentials for Am-type stars. The dependencies of
the relative abundances of chemical elements on the second ionization
potentials of these elements were investigated using the published
abundance patterns of B-F-type stars. The correlations of relative and
absolute abundances of chemical elements, second ionization
potentials, and projected rotational velocities are clearly detected
for stars with effective temperatures between 7000 and 12000K. If the
correlation of relative abundances and second ionization potentials
can be explained by the accretion of interstellar gas on the stellar
surfaces, the investigation of these correlations can provide valuable
information on the density and velocities of interstellar gas in
different regions of the Galaxy and also on the influence of this
phenomenon on stellar evolution. The dependencies of the relative
abundances of chemical elements on the condensation temperatures of
these elements were also found in the atmospheres of ρ Pup,
δ Sct, and other B--F-type stars. Ten possible λ Boo-type
stars were detected. The effective temperatures of these objects are
between 10900 and 14000K.
Description:
Observations of ρ Pup from the Very Large Telescope (VLT) archives
(Bagnulo, 2003Msngr.114...10B 2003Msngr.114...10B) were taken. These high-quality spectra
observed with the UVES spectroscope are the main source of information
about the atmospheric conditions in ρ Pup used in this paper. The
spectral resolving power is R=80000, the signal-to-noise ratio is more
than 300 in the red spectral region, and the wavelength coverage is
from 3040 to 10400Å with several gaps.
We also used 13 International Ultraviolet Explorer (IUE) spectra of
ρ Pup from the INES archive. The spectral resolving power of
International Ultraviolet Explorer (IUE) spectra is near R=18000, and
the wavelength coverage is from 1850 to 3350Å. The signal-to-noise
ratio is on the order of 10-20.
Objects:
----------------------------------------------------------
RA (ICRS) DE Designation(s)
----------------------------------------------------------
08 07 32.65 -24 18 15.6 * rho Pup = HIP 39757
----------------------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 40 167 Iron lines in the spectrum of ρ Pup
table2.dat 95 430 Abundances of chemical elements in the atmosphere
of ρ Pup: individual lines
table3.dat 83 73 Abundances of chemical elements in the atmosphere
of ρ Pup: mean values
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See also:
B/gcvs : General Catalogue of Variable Stars (Samus+ 2007-2013)
VI/69 : Atomic Spectral Line List (Hirata+ 1995)
J/AJ/145/167 : Abundances of LX Per (Kang+, 2013)
J/AJ/144/35 : Abundances of the eclipsing binary ZZ Boo (Kang+, 2012)
J/PASP/124/401 : Chemical composition of BE Lyn (Kim+, 2012)
J/AJ/134/926 : Chemical composition of V2314 Oph (Kim+, 2007)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Ion Iron line identifier (Fe I or Fe II)
7- 14 F8.3 0.1nm lambda [4620/8839] Wavelength λ; in Å
16- 20 F5.2 [-] loggf [-5.24/0.53] Log of the oscillator strength
22- 23 I2 --- r_loggf Reference for loggf (G2)
25- 30 F6.3 eV Elow [0/10.48] Lower level energy
32- 34 I3 0.1pm EW [4/198] Equivalent width; in mÅ
36- 40 F5.3 [-] logN [7.783/8.03] Log number abundance (G3)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 A3 --- Tel Telescope facility used (IUE or VLT) (G1)
5- 10 A6 --- Ion Species identifier
12- 19 F8.3 0.1nm lambda [1942/9797] Wavelength λ; in Å
21- 26 F6.3 [-] loggf [-5.69/1.29] Log of the oscillator strength
28- 29 I2 --- r_loggf Reference for loggf (G2)
31- 36 F6.3 eV Elow [0/12.729] Lower level energy
38- 43 F6.3 [-] logN* Log number absolute abundance in ρ Pup (G3)
45- 50 F6.3 [Sun] logNo ? Log number absolute abundance in the Sun (G3)
52- 57 F6.3 [Sun] Abund Difference between logN* and logNS (1)
59- 63 F5.3 --- Inp* Relative input of the investigated line to the
line absorption coefficient in synthetic spectrum
of ρ Pup (1=Clean line, 0=Very weak line) (2)
65- 69 F5.3 --- Inpo ? Relative input of the investigated line to the
line absorption coefficient in synthetic spectrum
of the Sun (1=Clean line, 0=Very weak line) (2)
71- 75 F5.3 --- Depth* Depth of line in synthetic spectrum of ρ Pup
77- 81 F5.3 --- Deptho ? Depth of line in synthetic spectrum of the Sun
83- 88 F6.3 [-] d(T) ? Change in logN* for Teff=+100K (3)
90- 95 F6.3 [-] d(g) ? Change in logN* for logg=-0.3 (3)
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Note (1): For lines with observed counterparts in the solar spectrum, the direct
difference between our determination of the abundances in the atmospheres
of ρ Pup and that of the Sun is given. If the line is absent in the
solar spectrum, the standard solar composition from Grevesse et al.
(2010Ap&SS.328..179G 2010Ap&SS.328..179G) was used to calculate the relative abundance.
Note (2): The relative input was calculated as the ratio of the line absorption
coefficient produced by the investigated line to the total line absorption
coefficient at the central wavelength of the investigated line. The
relative input changes from 1.0 for a clean line to 0.0 for very weak lines
with a strong input of absorption from other lines.
Note (3): These values can be used to estimate the errors in abundance
determinations that are due to the improper selection of atmospheric
parameters, variations of these parameters during the pulsation cycle, the
fitting procedure, and other uncertainties.
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 A3 --- Tel Telescope facility used (IUE or VLT) (G1)
5- 6 I2 --- Z [3/90] Atomic number
8- 13 A6 --- Ion Species identification
15- 17 I3 --- Nl [1/120] Number of lines used
19- 23 F5.2 [Sun] Abest Best value mean abundance (ρ Pup minus
Solar) (1)
25- 28 F4.2 [Sun] e_Abest ? 1σ uncertainty in Abest
30- 34 F5.2 [Sun] A+100K Mean abundance (ρ Pup minus Solar) with
effective temperature increased by +100K
36- 39 F4.2 [Sun] e_A+100K ? 1σ uncertainty in A+100K
41- 45 F5.2 [Sun] Ag+0.2 Mean abundance (ρ Pup minus Solar) with
surface gravity decreased by +0.2cm/s2
47- 50 F4.2 [Sun] e_Ag+0.2 ? 1σ uncertainty in Ag+0.2
52- 56 F5.2 [-] Nbest Best value of ρ Pup absolute mean
abundance (2)
58- 61 F4.2 [-] e_Nbest ? 1σ uncertainty in Nbest
63- 67 F5.2 [-] N+100K Absolute mean abundance of ρ Pup with
effective temperature increased by +100K
69- 72 F4.2 [-] e_N+100K ? 1σ uncertainty in N+100K
74- 78 F5.2 [-] Ng+0.2 Absolute mean abundance of ρ Pup with
surface gravity decreased by +0.2cm/s2
80- 83 F4.2 [-] e_Ng+0.2 ? 1σ uncertainty in Ng+0.2
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Note (1): Mean values of the relative abundances shown in the column 'Abund' of
Table 2 for the specified ion.
Note (2): Mean values of the column 'logN*' of Table 2.
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History:
From electronic version of the journal
Global Notes:
Note (G1): Telescope codes are:
IUE = International Ultraviolet Explorer (see Cat. VI/110)
VLT = Very Large Telescope.
Note (G2): Reference codes are defined as follows:
1 = Kurucz (1993sssp.book.....K 1993sssp.book.....K);
2 = Fuhr & Wiese (2006JPCRD..35.1669F 2006JPCRD..35.1669F);
3 = solar log(gf), this paper;
4 = Piskunov et al. (1995A&AS..112..525P 1995A&AS..112..525P).
5 = Kelleher & Podobedova (2008JPCRD..37..267K 2008JPCRD..37..267K);
6 = Ivans et al. 2006 (cat. J/ApJ/645/613);
7 = solar log(gf), this paper;
8 = Kurucz (1995KurCD..23.....K 1995KurCD..23.....K);
9 = Morton (2000ApJS..130..403M 2000ApJS..130..403M);
10 = Ljung et al. (2006A&A...456.1181L 2006A&A...456.1181L);
11 = Biemont et al. (2002, Database of Rare Earths At Mons University,
http://www.umh.ac.be/astro/dream.html);
12 = Den Hartog et al. (2003ApJS..148..543D 2003ApJS..148..543D);
13 = Piskunov et al. (1995A&AS..112..525P 1995A&AS..112..525P);
14 = Nilsson et al. (2002A&A...382..368N 2002A&A...382..368N);
15 = Kramida et al. (2014, NIST Atomic Spectra Database (version 4.0.0),
http://physics.nist.gov/asd);
16 = Hirata & Horaguchi 1995 (cat. VI/69);
17 = Kurucz & Peytremann 1975 (cat. VI/10).
Note (G3): In the scale logN(H)=12.
(End) Greg Schwarz [AAS], Sylvain Guehenneux [CDS] 10-Mar-2015