Erratum: He abundance in the ejecta of U Sco
MNRAS 448, 3414–3415 (2015)
doi:10.1093/mnras/stv243
Erratum: He abundance in the ejecta of U Sco
by M. P. Maxwell,1 M. T. Rushton,1 M. J. Darnley,2 H. L. Worters,3 M. F. Bode,2
A. Evans,4 S. P. S. Eyres,1‹ M. B. N. Kouwenhoven,5 F. M. Walter6
and B. J. M. Hassall1
1 Jeremiah
Horrocks Institute, University of Central Lancashire, Preston PR1 2HE, UK
Research Institute, Liverpool John Moores University, Birkenhead CH41 1LD, UK
3 South African Astronomical Observatory, PO Box 9, 7935 Observatory, South Africa
4 Astrophysics Group, Keele University, Keele, Staffordshire ST5 5BG, UK
5 Kavli Institute for Astronomy and Astrophysics, Peking University, Yi He Yuan Lu 5, Haidian Qu, Beijing 100871, China
6 Department of Physics and Astronomy, Stony Brook University, Stony Brook, NY 11794-3800, USA
2 Astrophysics
Key words: errata, addenda – circumstellar matter – infrared: stars.
Table 1. Corrected
numbers.
day
Published day
Correct day
1.93
4.93
5.41
5.93
6.81
7.81
7.93
8.81
8.93
9.43
9.93
10.93
11.81
11.93
12.81
1.94
4.95
6.16
5.93
7.07
8.04
7.91
9.04
8.91
9.43
9.90
10.92
12.04
11.90
13.08
The revised component abundance estimates and associated errors for each line are shown in Table 2. The weighted mean
Table 2. Revised helium abundances,
to replace table 6 in the original paper.
Helium line
Derived abundance
He I 6678 Å
He II 4686 Å
He II 5411 Å
He II 1.163 µm
figs 1–4 were listed incorrectly. These were discovered during the
viva of the lead author, and were simple arithmetic errors; the data
were correctly reduced and the measurements were conducted correctly.
Table 1 shows the correspondence between the published day
numbers and the correct day numbers. Note that the order of the
observations changes at two points: day 5.93 moves from fourth to
third observation, and the penultimate observation moves to third
from last, swapping with the one previously listed as third from last.
This does not affect the discussion or any of the conclusions of the
paper.
0.061 ± 0.01
0.047 ± 0.008
0.076 ± 0.014
0.061 ± 0.010
abundance
from
the
ionized
helium
lines
is
N(He)/N(H)=0.056 ± 0.019 with the errors added in quadrature.
Combined with the abundance from the neutral line, this gives a
total abundance of N(He)/N(H)=0.117 ± 0.014.
We note that this is closer to the results of Iijima (2002), who
found N(He)/N(H)=0.16 ± 0.02 purely from He I lines. The 3σ
range of this value is within 3σ range of our value. However, Iijima
(2002) employed indirect arguments to determine which of the
ratios they discuss was the best representation of the true value. Our
work is the first direct measurement incorporating both He I and
He II lines and hence the most robust determination to date.
Using the Asplund, Grevesse & Sauval (2005) solar abundance
value of N(He)/N(H) = 0.085, we find an overabundance relative to
solar to be a factor of 1.38±0.15. This is well within the range for
typical classical novae (table 6.1 of José & Shore 2008) showing
that this recurrent nova with a main-sequence-type secondary shows
no particular helium enhancement compared to these very similar
binary systems.
We confirm the original conclusion that previously claimed overabundance of helium was due to incomplete sampling of the neutral
and ionized lines, and was not due to a helium-rich secondary.
AC K N OW L E D G E M E N T S
E-mail:
We thank Professor G. E. Bromage and Dr B. Smalley for identifying these errors.
C 2015 The Authors
Published by Oxford University Press on behalf of the Royal Astronomical Society
The paper ‘The helium abundance in the ejecta of U Scorpi’ was
published in MNRAS, 419, 1465 (2012).
An error has been identified in the abundance calculations, including the error analysis. In addition, the day numbers presented
in Table 1 and used to identify observations in tables 2–5 and
Erratum: The helium abundance in the ejecta of U Scorpii
REFERENCES
Asplund M., Grevesse N., Sauval A. J., 2005, in Thomas G. B., III Frank
N. B., eds, ASP Conf. Ser., Vol. 336, Cosmic Abundances as Records
of Stellar Evolution and Nucleosynthesis in honor of David L. Lambert.
Astron. Soc. Pac., San Francisco, p. 25
Iijima T., 2002, A&A, 387, 1013
3415
José J., Shore S. N., 2008, in Bode M. F., Evans A., eds, Classical Novae.
Cambridge Univ. Press, Cambridge, p. 121
This paper has been typeset from a TEX/LATEX file prepared by the author.
MNRAS 448, 3414–3415 (2015)
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