ChemInform Abstract: Synthesis of S,S‐Dimethylsulfilimino‐Substituted Azines.

Filatov, I. E.; Kulikov, Yu. V.; Pusinov, G. L.; Pashkevich, K. I.

doi:10.1002/chin.199020216

ChemInform

1990

DOI: 10.1002/chin.199020216

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ChemInform Abstract: Synthesis of S,S‐Dimethylsulfilimino‐Substituted Azines.

I. E. Filatov

Yu. V. Kulikov

G. L. Pusinov

et al.

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2017

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“…Filatov (1960); (3)Pócs & Szeidl (2001); (4)Broglia & Conconi (1975);(5)Braune et al (1979); (6) Braune & Mundry (1982); (7) Huebscher et al (1985); (8) Rodriguez et al (1992); (9) Hübscher et al (1992); (10) Hintz et al (1997a); (11) Agerer et al (1999b); (12) Agerer et al (1999a); (13) Pejcha et al (2001); (14) Zhou (2001); (15) Agerer & Hubscher (2003); (16)Hubscher (2005); (17) Hubscher et al (2005); (18) Klingenberg et al (2006); (19) Hubscher et al (2006); (20) Hubscher & Walter (2007); (21) Samolyk (2010); (22) Hubscher (2007); (23) Hubscher et al (2009); (24) Hubscher et al (2010); (25) Huebscher & Monninger (2011); (26) this work.…”

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AE Ursae Majoris – a δ Scuti Star in the Hertzsprung Gap

Niu

et al. 2017

Mon. Not. R. Astron. Soc.

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We analyze the photometric data and spectroscopic data that collect on the δ Scuti star AE UMa. The fundamental and the first overtone frequencies are confirmed as f 0 = 11.62560 c d −1 and f 1 = 15.03124 c d −1 , respectively, from the frequency content by analyzing of the 40 nights light curve spanning from 2009 to 2012. Additionally, another 37 frequencies are identified as either the harmonics or the linear combinations of the fundamental and the first overtone frequencies, among which 25 are newly detected. The rate of period change of the fundamental mode is determined as (1/P 0 )(dP 0 /dt) = 5.4(±1.9) × 10 −9 yr −1 as revealed from the O − C diagram based on the 84 newly determined times of maximum light combined with those derived from the literature. The spectroscopic data suggests that AE UMa is a population I δ Scuti star. With these physical properties, we perform theoretical explorations based on the stellar evolution code MESA on this target, considering that the variation of pulsation period is caused by secular evolutionary effects. We finally constraint the AE UMa with the physical parameters as: the mass of 1.805 ± 0.055 M ⊙ , the radius of 1.647 ± 0.032 × 10 11 cm, the luminosity of 1.381 ± 0.048 (log L/L ⊙ ) and the age of 1.055 ± 0.095 × 10 9 yr. AE UMa can be the (Pop. I) δ Scuti star that locates just after the second turn-off of its evolutional track leaving the main sequence, a star in the phase of the Hertzsprung Gap with a helium core and a hydrogen-burning shell.

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AE Ursae Majoris – a δ Scuti Star in the Hertzsprung Gap

Niu

et al. 2017

Mon. Not. R. Astron. Soc.

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ChemInform Abstract: Synthesis of S,S‐Dimethylsulfilimino‐Substituted Azines.

Cited by 1 publication

References 0 publications

AE Ursae Majoris – a δ Scuti Star in the Hertzsprung Gap

AE Ursae Majoris – a δ Scuti Star in the Hertzsprung Gap

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