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Table 2

Summary of optical spectra of Var C.

Date JD Features Spectral type Ref.

30 Nov. 1946 2 432 155 Ca ii K and Ca ii H in absorption with later than F0 1
nearly equal strength
Hγ and Hδ weakly in absorption
23 Aug. 1947 2 432 421 Ca ii K and Ca ii H in absorption with later than F0 1
nearly equal strength
24/25 July–22 Sept. 1949 2 433 122–2 433 182 faint Hβ in emission 1
3 Aug.–28/31 Oct. 1951 2 433 862–2 433 951 Hβ and Hγ in emission late A-typea 1
Ca ii K and Ca ii H in absorption
29 Nov. 1951 2 433 980 Hβ and Hγ in emission 1
27/28 Sept. 1973 2 441 953 bright Hα in emission 2
14 Oct.–10 Nov. 1974 2 442 335–2 442 362 several hydrogen, He i  Fe ii, late B-typea 3
and [Fe ii] lines in emission
Ca ii K in absorption
Aug. 1976 2 443 006 compared to previous spectrum: early B-typea 4
hydrogen and He i emission lines weaker
some of the Fe ii and [Fe ii] lines no longer seen
10/11 Nov. 1983 2 445 649.5 Hα, Hγ and numerous Fe ii lines in emission A-typea 5
all with P-Cygni profiles
strong Mg iiλ4481 in absorption
Nov.–Dec. 1985 2 446 385–2 446 415 Hα and Hβ in emission F0Ia–F5Ia 6
several strong Fe ii and
ionised metal lines in absorption
I(Ca ii K) >I(Ca ii H + Hϵ)
Aug.–Sept. 1986 2 446 658–2 446 689 weaker metallic lines A2–A3 6
I(Ca ii H + Hϵ) >I(Ca ii K)
15/16/17 Sept. 1987 2 447 054–2 447 056 Fe ii and other metallic lines in absorption A-type 6
several Fe ii-lines in emission
Hα, Hβ, and Hγ showed P-Cygni profiles
3/6 Oct.–13 Dec. 1992 2 448 899–2 448 970 weak He i lines in absorption late B-typea 7
compared to previous spectra:
hydrogen and Fe ii emission lines getting stronger
14/15 Dec. 1993 2 449 336.5 pronounced hydrogen lines in emission late B-typea 8
several Fe ii and [Fe ii] lines in emission
weak He i line
30 Nov. 2003 2 452 974 Hβ in emission and numerous metallic lines F0Ia–F5Ia 9
in absorption
13 Nov. 2004 2 453 323 Hα, Hβ, and Hγ in emission, some weak Fe i A-type 10
lines in absorption or emission
7/8 Dec. 2004–16 Jan. 2005 2 453 347–2 453 387 strong hydrogen lines in emission B[e] 11
several Fe ii and [Fe ii] lines in emission
22 Oct. 2008 2 454 762 Hα and Hβ, in emission, some He i lines and B-type 10
several Fe i lines in emission
29 Sept.–2 Oct. 2010 2 455 469–2 455 472 Hα, Hβ, and Hγ in emission, several He i and B-typea 9
Fe ii lines in emission, P-Cygni profiles
3 Oct. 2010 2 455 473 hydrogen, He i, Fe ii, and [Fe ii] lines in emission, B1–B2 12
P-Cygni profiles
18 Sept. 2013 2 456 554 hydrogen lines in emission A-typea 13
5 Oct. 2013 2 456 571 Fe ii, [Fe ii], and strong hydrogen lines in emission, late B-typea 14
P-Cygni profiles
He i very weakly in absorption
7 Oct. 2013 2 456 573 hydrogen in emission (weaker than in 10/2010), late A-type 12
Ca ii and Mg ii in absorption,
Fe ii in emission with P-Cygni profiles
1/2 Nov. 2013 2 456 598.5 Fe ii, [Fe ii], and strong hydrogen lines in emission, late B-typea 14
P-Cygni profiles
He i very weakly in absorption

Notes.

(a)

Estimated spectral type based upon the description of the spectrum.

Reference. (1) Hubble & Sandage (1953); (2) Sharov et al. (1975); (3) Humphreys (1975); (4) Humphreys (1978); (5) Kenyon & Gallagher (1985); (6) Humphreys et al. (1988); (7) Szeifert et al. (1996); (8) Massey et al. (1995); (9) Clark et al. (2012); (10) this paper; (11) Viotti et al. (2006); (12) Humphreys et al. (2014); (13) Viotti et al. (2013); (14) Valeev et al. (2013).

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