J/ApJ/877/75 BVRI photom. of DV Psc and known short-period EBs (Pi+, 2019)
Magnetic activity and orbital period study for the short-period RS CVn-type
eclipsing binary DV Psc.
Pi Q.-F., Zhang L.-Y., Bi S.-L., Han X.L., Lu H.-P., Yue Q., Long L., Yan Y.
<Astrophys. J., 877, 75 (2019)>
=2019ApJ...877...75P 2019ApJ...877...75P
ADC_Keywords: Binaries, eclipsing; Photometry, UBVRI; Stars, flare;
Spectral types
Keywords: binaries: eclipsing ; stars: chromospheres ; stars: flare ;
stars: individual (DV Psc) ; starspots
Abstract:
Using 27 sets of new multiband photometry light curves acquired from
our long-term photometric campaign carried out in the last 5yr and
high-resolution spectroscopic data from seven nights, we analyzed the
physical mechanisms of period variation, starspot cycle, optical
flares, and chromospheric activities of the eclipsing binary DV Psc.
Our updated O-C diagram covering a period of approximately 20yr shows
an oscillation in its orbital period. This variations might be caused
by a third body with an orbital period of 14.58±0.28yr. There are
two active regions of starspots at longitude belts of about 90°
and 270°. We obtained its starspot cycles with periods of
3.60±0.03yr and 3.42±0.02yr at about 90° and 270°,
respectively. Moreover, the magnitude difference of Max.I-Max.II shows
cyclic oscillation of 5.15±0.01yr. During our decade long
photometric campaign, we observed DV Psc a total of 326.4hr, detected
18 outbursts (12 of them have never been reported) with flare energies
in the range of (6.62-1106.85)x1024J. The slope of the relationship
between the phase of the max flare and spots is 0.842 ±0.083,
implying a correlation between spots and flares. We discovered
evidence for a correlation between the rotation period and the
activity cycle for the short-period eclipsing binaries. Our
high-resolution spectroscopic observations of DV Psc show obvious
emissions above continuum in the Hα line and small self-reversal
emissions of the CaII IRT lines.
Description:
We carried out our new multicolor CCD photometric campaign of DV Psc
using a multitude of telescopes from Asia, North and South America,
and Europe: the 85cm and 60cm telescopes located at Xinglong station
of the National Astronomical Observatories of China (XL85T, XL60T, and
NAOC); the 100cm telescope (YN100T) located at Yunnan Observatory in
Kunming, China; the 91cm SARA (Southeastern Association for Research
in Astronomy) telescope (KPT) located at the Kitt Peak National
Observatory in Arizona, USA; the SARA 61cm telescope (CT) at the Cerro
Tololo Inter-American Observatory in Chile; the 100cm SARA RM
telescope (RMT) at the observatory del Roque de los Muchachos, La
Palma, Spain; and the 95cm Holcomb telescope at the Holcomb
Observatory (HT) on the Bulter University campus in Indianapolis,
Indiana, USA. We observed DV Psc for 67 nights (about 326.4hr) from
2013 November 20 to 2018 January 28 using the standard BVRI filters;
the exposure times are 15-45s, 5-30s, 3-10s, and 1-7 s in BVRI
filters, respectively.
We listed the photometry observation log in Table 1.
We obtained high-resolution spectra (HRS; R=49800) for DV Psc during
seven nights (2017 January 3, 4, 11, 12, 13, 14, and 17) using the
echelle spectrograph on the 2.16m telescope of NAOC.
Objects:
----------------------------------------------------------
RA (ICRS) DE Designation(s)
----------------------------------------------------------
00 13 09.20 +05 35 43.0 DV Psc = TYC 8-324-1
----------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 109 9755 BVRI photometric data of DV Psc
table9.dat 74 37 Flares detected in DV Psc and their parameters
table13.dat 131 206 All known short-period eclipsing binaries
system with cycles
refs.dat 73 167 References
--------------------------------------------------------------------------------
See also:
J/AJ/108/268 : HK survey emission-line candidates positions (Beers+ 1994)
J/A+A/285/459 : RZ Dra (Kreiner+ 1994)
J/A+AS/146/103 : CaII H&K to CaII IRT echelle spectra (Montes+, 2000)
J/MNRAS/328/45 : Late-type stars members of young groups (Montes+, 2001)
J/A+A/393/225 : Starspot cycles of 6 young solar analogues (Messina+, 2002)
J/A+A/424/993 : BH Vir spectra and photometry (Kjurkchieva+, 2004)
J/AJ/131/2986 : Multiplicity of contact binaries (Pribulla+, 2006)
J/MNRAS/379/1665 : XX Cep BVRI light curves (Lee+, 2007)
J/A+A/465/943 : BVI and RV curves of 5 eclipsing binaries (Szalai+, 2007)
J/AJ/136/594 : BS Cas BVR light curves (Yang+, 2008)
J/AJ/137/3181 : HW Vir differential VR light curves (Lee+, 2009)
J/MNRAS/406/2559 : BVRI light curves of GSC2314-0530 (Dimitrov+, 2010)
J/AJ/139/1360 : AO Ser VR light curves (Yang+, 2010)
J/AJ/142/99 : BVRI observations of TZ Boo (Christopoulou+, 2011)
J/AJ/141/44 : V396 Mon BVRI light curves (Liu+, 2011)
J/PASP/123/895 : EH Cnc RV light curves (Yang+, 2011)
J/AJ/144/149 : CCD photom. of the W UMa type TY Boo (Christopoulou+, 2012)
J/other/NewA/17.347 : Eclipsing times of BE Cep (Dai+, 2012)
J/AJ/143/122 : VR light curves of CK Boo (Yang+, 2012)
J/AJ/145/100 : Differential BVR light curves of EP And (Lee+, 2013)
J/AJ/145/60 : Light curves of GN Boo, BL Leo, and V1918 Cyg (Yang+, 2013)
J/AJ/146/35 : BVR light curves of DZ Psc (Yang+, 2013)
J/AJ/145/39 : Differential BV(RI)c light curves of PY Vir (Zhu+, 2013)
J/AJ/147/98 : Times of minimum light for EQ Tau (Li+, 2014)
J/AJ/147/50 : Differential BVRI light curves of DV Psc (Pi+, 2014)
J/MNRAS/442/2620 : VRI light curve of 5 eclipsing binaries (Zhang+, 2014)
J/other/NewA/36.50 : V873 Per BVR light curves (Kriwattanawong+, 2015)
J/other/NewA/41.17 : Time of minima of BX Peg (Li+, 2015)
J/AJ/150/9 : VRI light curves of GSC 1537-1557 (Xiang+, 2015)
J/AJ/149/62 : BVR light curves of V508 Oph (Xiang+, 2015)
J/other/NewA/37.48 : ZZ Cyg times of minima (Yang+, 2015)
J/other/NewA/48.58 : V1044 Her VR differential photometry (Lu+, 2016)
J/AJ/153/137 : New NSVS 14256825 eclipse times (Nasiroglu+, 2017)
J/AJ/154/260 : 3 short-period eclipsing binaries BVRI photom. (Pi+, 2017)
J/ApJ/835/251 : RVs and BVIc LCs of the EB* CU Cnc (Wilson+, 2017)
J/other/NewA/55.13 : UY UMa and EF Boo compiled time of minima (Yu+, 2017)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- Date Observation date code
21- 32 F12.4 d HJD-B ? Heliocentric Julian Date of B band observation
35- 40 F6.3 mag DelBmag [-1.3/-0.12]? Differential B band magnitude
44- 55 F12.4 d HJD-V ? Heliocentric Julian Date of V band observation
58- 63 F6.3 mag DelVmag [-0.91/0.83]? Differential V band magnitude
67- 78 F12.4 d HJD-R ? Heliocentric Julian Date of R band observation
81- 86 F6.3 mag DelRmag [-1.1/-0.4]? Differential R band magnitude
90-101 F12.4 d HJD-I ? Heliocentric Julian Date of I band observation
104-109 F6.3 mag DelImag [-1.3/-0.8]? Differential I band magnitude
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table9.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 "Y/M/D" Date UT date of observation
13- 24 F12.5 d HJDmax [7647.7/58069.54] The time of maximum
brightness; HJD-2400000
26- 29 F4.2 --- Phase [0.09/0.95] The phase according to
ephemeris (1) of maximum brightness
31- 34 F4.2 --- Spot [0.14/0.98] Spot phase
36- 37 A2 --- Filt Filter
39- 42 F4.1 min Rise [0.4/13] The rise time of the flare
44- 47 F4.1 min Decay [1.3/15.1] The decay time of the flare
49- 52 F4.1 min Dur [1.8/22.3] The duration of the flare
54- 58 F5.3 mag Amp [0.014/0.74] The brightening amplitude
(Δm)
60- 66 F7.2 10+24J Energy [6.6/1107] Estimated energy
68- 73 A6 --- Tel Telescope (1)
74 A1 --- f_Tel Flag on Tel (2)
--------------------------------------------------------------------------------
Note (1): Telescope as follows:
CT = the SARA 61cm telescope at the Cerro Tololo Inter-American
Observatory in Chile
HT = the 95cm Holcomb telescope at the Holcomb Observatory on the Bulter
University campus in Indianapolis, Indiana, USA.
RMT = the 100cm SARA RM telescope at the observatory del Roque
de los Muchachos, La Palma, Spain
XL85T = the 85cm telescope located at Xinglong station of the National
Astronomical Observatories of China
YN100T = the 100cm telescope located at Yunnan Observatory in Kunming, China
Note (2): Flag as follows:
a = Referenced Zhang et al. (2010NewA...15..362Z 2010NewA...15..362Z).
b = Referenced Pi et al. (2014, J/AJ/147/50).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table13.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Type Cycle type ("Single" or "Complex"=multi-cycles)
9- 21 A13 --- ID Identifier
23- 34 A12 --- SpType Spectral type
36- 43 A8 --- EBs Eclipsing binary type (1)
45- 53 F9.7 d PRot [0.06/8] Rotational period
55- 56 I2 d e_PRot [0/30]? Uncertainty in the last digits of PRot
58- 63 F6.2 yr P1 [1/181] First period
65- 69 F5.2 yr e_P1 [1/90]? Uncertainty in P1
71- 75 F5.2 yr P2 [1.8/88.4]? Second period; if available
77- 81 F5.2 yr e_P2 [1/90]? Uncertainty in P2
83- 87 F5.2 yr P3 [2/22.8]? Third period; if available
89- 93 F5.2 yr e_P3 [3/29]? Uncertainty in P3
95- 99 F5.2 yr P4 [10.5/13]? Fourth period; if available
101-104 F4.2 yr P5 [7.65]? Fifth period; if available
106-109 F4.2 yr P6 [9.23]? Sixth period; if available
111-123 A13 --- Method Method used (2)
125-131 A7 --- Ref Reference code(s) (see refs.dat file)
--------------------------------------------------------------------------------
Note (1): Eclipsing binary type as follows:
W UMa = W UMa type (78 occurrences);
Algol = Algol type (73 occurrences);
Ca V = Cataclysmic variable (23 occurrences);
RS CVn = RS CVn binary (14 occurrences);
Beta Lyr = β Lyr type (12 occurrences);
LEB = low-mass eclipsing binary (2 occurrences);
Am Her = 1 occurrence;
Be Star = 1 occurrence;
HM Vir = 1 occurrence;
RR Lyr = 1 occurrence.
Note (2): Method used as follows:
Pv = Period variations;
Spmv = Spot phase migration variations;
Bv = Brightness variations;
Cv = Color variations.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: refs.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I03 --- Ref Reference code
5- 23 A19 --- BibCode Bibcode of the reference
25- 48 A24 --- Auth First author's name(s)
50- 73 A24 --- Comm Comment
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 23-Nov-2020