J/ApJ/795/8 Nova CI Aql MMO light curve data (Wilson+, 2014)
Outburst-related period changes of recurrent nova CI Aquilae.
Wilson R.E., Honeycutt R.K.
<Astrophys. J., 795, 8 (2014)>
=2014ApJ...795....8W 2014ApJ...795....8W (SIMBAD/NED BibCode)
ADC_Keywords: Novae ; Magnitudes
Keywords: novae, cataclysmic variables - stars: individual: CI Aql
Abstract:
Pre-outburst and post-outburst light curves and post-outburst eclipse
timings are analyzed to measure any period (P) change related to
nova CI Aql's outburst of early 2000 and a mean post-outburst dP/dt, which
then lead to estimates of the accreting component's rate of mass (M)
change and its overall outburst-related change of mass over roughly a
decade of observations. We apply a recently developed procedure for
unified analysis of three timing-related data types (light curves,
radial velocities, and eclipse timings), although with only light
curves and timings in this case. Fits to the data are reasonably good
without need for a disk in the light-curve model, although the disk
certainly exists and has an important role in our post-outburst mass
flow computations. Initial experiments showed that, although there
seems to be an accretion hot spot, it has essentially no effect on
derived outburst-related ΔP or on post-outburst dP/dt. Use of
atomic time (HJED) in place of HJD also has essentially nil effect
on ΔP and dP/dt. We find ΔP consistently negative in
various types of solutions, although at best only marginally
significant statistically in any one experiment. Pre-outburst HJD0
and P results are given, as are post-outburst HJD0, P, and dP/dt,
with light curves and eclipse times as joint input, and also with only
eclipse time input. Post-outburst dP/dt is negative at about
2.4σ. Explicit formulae for mass transfer rates and
epoch-to-epoch mass change are developed and applied. A known offset
in the magnitude zero point for 1991-1994 is corrected.
Description:
All of the MMO images were in the V band, with exposure times of
2-4 minutes. A full description of the MMO unattended facility, the
data acquisition process, the data reductions, and the observing
programs is in Honeycutt et al. (2013, J/PASP/125/126, hereafter H13).
The pre-outburst data were acquired with the MMO 0.41 m telescope and
a liquid nitrogen cooled CCD (Campaigns A and B in H13). The
post-outburst data were acquired with the 1.25 m and 0.41 m telescopes
at the MMO, each with thermo-electrically cooled CCDs (Campaigns C-E
in H13). The four campaigns were reduced independently because the
transformation coefficients and the CCD sizes differed. Averaged
across all campaigns, about 75 comparison stars were used in each
ensemble solution, resulting in a mean error for CI Aql of 0.04 mag.
Objects:
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RA (ICRS) DE Designation(s)
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18 52 03.57 -01 28 39.4 CI Aql = NOVA Aql 1917
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 26 594 CI Aql MMO Light Curve Data
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See also:
J/AJ/140/34 : Classification of nova light curves (Strope+, 2010)
J/A+A/544/A26 : CI Aql spectra during 2000 outburst (Iijima, 2012)
J/PASP/125/126 : Light curve of CR Boo over 1990-2012 (Honeycutt+, 2013)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 F11.5 d HJD Heliocentric Julian Date (HJD-2400000)
13- 18 F6.3 mag Vmag The V band magnitude
20- 24 F5.3 mag e_Vmag Standard deviation in Vmag
26 A1 --- Campaign [ABCDE] Campaign identifier (1)
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Note (1): Identified as follows:
A, B = The pre-outburst data were acquired with the MMO 0.41 m telescope
and a liquid nitrogen cooled CCD;
C, D, E = The post-outburst data were acquired with the 1.25 m and 0.41 m
telescopes at the MMO, each with thermo-electrically cooled CCDs.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 17-May-2017