J/ApJ/897/48 Properties of Galactic Be Supergiants. VI. (Miroshnichenko+, 2020)
Properties of Galactic B[e] Supergiants.
VI. 3 Pup-Constraining the Orbital Parameters and Modeling the Circumstellar
Environments.
Miroshnichenko A.S., Danford S., Zharikov S.V., Klochkova V.G.,
Chentsov E.L., Vanbeveren D., Zakhozhay O.V., Manset N., Pogodin M.A.,
Omarov C.T., Kuratova A.K., Khokhlov S.A.
<Astrophys. J., 897, 48 (2020)>
=2020ApJ...897...48M 2020ApJ...897...48M
ADC_Keywords: Stars, A-type; Stars, Be; Stars, supergiant; Spectra, optical;
Spectra, infrared; Radial velocities
Keywords: Emission line stars ; Binary stars ; High resolution spectroscopy
Abstract:
We report the results of long-term spectroscopic monitoring of the
A-type supergiant with the B[e] phenomenon 3Pup=HD62623. We confirm
earlier findings that it is a binary system. The orbital parameters
were derived using cross-correlation of the spectra in a range of
4460-4632Å, which contains over 30 absorption lines. The orbit was
found to be circular with a period of 137.4±0.1days, radial
velocity semiamplitude K1=5.0±0.8km/s, systemic radial velocity
γ=26.4±2.0km/s, and mass function
f(m)=(1.81-0.76+0.97)x10-3M☉. The object may have evolved
from a pair with initial masses of ∼6.0M☉ and ∼3.6M☉ with an
initial orbital period of ∼5days. Based on the fundamental parameters
of the A-supergiant (luminosity log L/L☉=4.1±0.1 and effective
temperature Teff=8500±500K) and evolutionary tracks of
mass-transferring binaries, we found current masses of the gainer
M2=8.8±0.5M☉ and donor M1=0.75±0.25M☉. We also modeled
the object's IR-excess and derived a dust mass of ∼5x10-5M☉ in
the optically thin dusty disk. The orbital parameters and properties
of the Hα line profile suggest that the circumstellar gaseous
disk is predominantly circumbinary. The relatively low mass of the
gainer led us to a suggestion that 3 Pup should be excluded from the
B[e] supergiant group and moved to the FSCMa group. Overall these
results further support our original suggestion that FSCMa objects are
binary systems, where an earlier mass transfer caused formation of the
circumstellar envelope.
Description:
Observations of 3 Pup are summarized in table1.
Objects:
-------------------------------------------------------
RA (2000) DE Designation(s) (Period)
-------------------------------------------------------
07 43 48.47 -28 57 17.4 3 Pup = HD 62623 (P=137.4d)
-------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 128 6 Observatories and instruments used for spectroscopic
observations
table2.dat 70 147 Log of spectroscopic observations of 3 Pup
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See also:
II/188 : Long-term photometry of Variables II (Sterken+, 1993)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/A+A/487/1129 : Evolutionary models of binaries (Van Rensbergen+, 2008)
J/other/AstBu/65.150 : Spectral line identification in 3 Pup (Chentsov+, 2010)
J/A+A/537/A146 : Stellar mod. with rotation. 0.8<M<120, Z=0.014 (Ekstrom+,2012)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 A4 --- Obs.ID Observatory identifier
6- 83 A78 --- Tel Telescope identifier
85- 98 A14 --- Inst Instrument used
100-104 I5 --- R [12000/65000]? Spectral resolution
106-128 A23 --- Place Instrument location
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 "month" Obs.M Month of the observation
4- 5 I2 d Obs.D Day of the observation
7- 8 I2 yr Obs.Y [04/20] Year of the observation
10 A1 --- Flag Observation flag (1)
12- 19 F8.3 d HJD [3365/8935] Heliocentric Julian Date; JD-24500000
21- 24 A4 --- Obs.ID Instrument used for observation
26- 29 I4 0.1nm LoWave [3600/5160] Lower spectral range wavelength (Å)
31- 35 I5 0.1nm UpWave [5279/10500] Upper spectral range wavelength (Å)
37- 41 F5.3 --- Phase [0/1] Orbital phase (2)
43- 46 F4.1 km/s RVel [-8.5/7.1]? Radial velocity (3)
48- 50 F3.1 km/s e_RVel [0.1/0.5]? The 1σ uncertainty in RVel
52- 55 F4.2 --- IV [1.5/2.26]? Blue peak intensity (4)
57- 60 F4.2 --- IR [2.12/3.3]? Red peak intensity (4)
62- 65 F4.2 --- Id [0.73/1.48]? Central depression intensity (4)
67- 70 F4.2 --- V/R [0.54/0.86]? Peak intensity ratio
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Note (1): Flags as follows:
a = a large portion or the entire cross-correlation region was not observed
(9 occurrences)
b = a systematic error in the wavelength calibration (5 occurrences)
c = region damaged by reflection on the CCD chip (3 occurrences)
Note (2): According to the RV solution (see text).
Note (3): Derived by cross-correlation in the range 4460-4632Angstroms with
respect to the template spectrum of 02/17/2017 (see Fig.1).
Note (4): In continuum units.
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History:
From electronic version of the journal
References:
Miroshnichenko et al. Paper I : 2002A&A...390..627M 2002A&A...390..627M
Miroshnichenko et al. Paper II : 2003A&A...406..673M 2003A&A...406..673M
Miroshnichenko et al. Paper III : 2004A&A...417..731M 2004A&A...417..731M
Miroshnichenko et al. Paper IV : 2005A&A...436..653M 2005A&A...436..653M
Men'Shchikov et al. Paper V : 2005A&A...443..211M 2005A&A...443..211M
(End) Prepared by [AAS], Coralie Fix [CDS], 27-Sep-2021