期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 436, 期 3, 页码 2082-2095出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stt1713
关键词
stars: AGB and post-AGB; binaries: general; stars: chemically peculiar; planetary nebulae: individual: LoTr 1; planetary nebulae: individual: WeBo 1; planetary nebulae: individual: A66 70
资金
- STFC
- ESO
- Marie Curie Actions of the European Commission (FP7COFUND)
- NASA [NAS5-26555]
- NASA Office of Space Science [NNX09AF08G]
- ESO telescopes at the La Silla Paranal Observatory [0.74.D-0373(A), 087.D-0174(A), 087.D-0205(A), 088.D-0750(A), 0.88D-0573(A), 0.89D-0453(A)]
- Science and Technology Facilities Council [ST/K006126/1, ST/J001562/1, ST/I001425/1, ST/I001719/1] Funding Source: researchfish
- STFC [ST/I001425/1, ST/J001562/1, ST/I001719/1, ST/K006126/1] Funding Source: UKRI
LoTr 1 is a planetary nebula thought to contain an intermediate-period binary central star system (that is, a system with an orbital period, P, between 100 and, say, 1500 d). The system shows the signature of a K type, rapidly rotating giant and most likely constitutes an accretion-induced post-mass-transfer system similar to other PNe, such as LoTr 5, WeBo 1 and A70. Such systems represent rare opportunities to further the investigation into the formation of barium stars and intermediate-period post-asymptotic giant branch systems - a formation process still far from being understood. Here, we present the first detailed analyses of both the central star system and the surrounding nebula of LoTr 1 using a combination of spectra obtained with Very Large Telescope-Focal Reducer and low dispersion Spectrograph, Anglo-Australian Telescope-UCL Coude Echelle Spectrograph and New Technology Telescope-European Southern Observatory Multi-Mode Instrument, as well as SuperWASP (Wide Angle Search for Planets) photometry. We confirm the binary nature of the central star of LoTr 1 that consists of a K1 III giant and a hot white dwarf. The cool giant does not present any sign of s-process enhancement but is shown to have a rotation period of 6.4 d, which is a possible sign of mass accretion. LoTr 1 also presents broad double-peaked H alpha emission lines, whose origin is still unclear. The nebula of LoTr 1 consists in two slightly elongated shells, with ages of 17 000 and 35 000 yr, respectively, and with different orientations. As such, LoTr 1 present a very different nebular morphology than A70 and WeBo 1, which may be an indication of difference in the mass-transfer episodes.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据