Skip to content
DraconiticResearch
Search Sources API
197,768 studies31 sourcesUpdated 54 min ago
PreprintCC BY 4.0arXiv

V405 Draconis: A Deep Contact Binary with a Tertiary Companion and a Quadruple System Candidate

  • Maksym Yu. Pyatnytskyy
  • Ivan L. Andronov
Open at sourcePDFDOICite

Abstract

We continued our analysis of the O-C diagram of the EW-type eclipsing binary V405 Dra using recently available data. We refined the orbital parameters of the third body responsible for the short-period oscillations in the O-C curve, obtaining P3=513.12(20) d, a12sin i3=0.3862(15) AU, and e3=0.1690(48). Assuming a total mass of $1.56$ M⊙ for the eclipsing binary, the minimum mass of the third body is estimated to be about $0.5$ M⊙. We also investigated the complex long-term O-C trend and found that it may be partially explained by the light-time effect caused by a possible fourth body, with a characteristic period of about 23.5 yr and a minimum mass of about $0.9$ M⊙. However, the fourth-body model cannot fully reproduce the observed long-term variation, particularly the earliest data, and the nature of part of the long-term trend remains unexplained.

Related

  1. V1374 Tau: A Dwarf Eclipsing Binary with Starspots, a Superflare, and a Tertiary Companion
    Yuangui Yang, Shuang Wang, Huiyu Yuan
    The Astrophysical JournalPeer-reviewedCC BY 4.0Full textSolar & stellar physicsIOP/AASCrossref
  2. A Search for Exoplanets around Northern Circumpolar Stars. XI. A Planetary Companion around HD 112987 and a Planetary Companion Candidate around HD 58545
    Byeong-Cheol Lee, Shenghong Gu, Beomdu Lim +6
    The Astronomical JournalPeer-reviewedCC BY 4.0Full textSolar & stellar physicsCrossref
  3. Asteroseismology and interferometry of the F7V spectroscopic binary χ Draconis A in the TESS CVZ
    Jonatan Rudrasingam, Mikkel N. Lund, Frank Grundahl +26
    Astronomy & AstrophysicsPeer-reviewedPublisher terms1 citedSolar & stellar physicsCrossref
  4. Asteroseismology and interferometry of the F7V spectroscopic binary χ Draconis A in the TESS CVZ
    Jonatan Rudrasingam, Mikkel N. Lund, Frank Grundahl +26
    arXivPreprintarXiv licenceFull textSolar & stellar physicsarXiv
  5. Companion architectures of sub-Saturns: Distinct migration pathways across the Neptunian landscape
    Luis Thomas, Louise D. Nielsen, Alex J. Cridland +2
    Astronomy & AstrophysicsPeer-reviewedPublisher terms1 citedSolar & stellar physicsCrossref

Cite

BibTeXRIS
BibTeX
@misc{pyatnytskyy2026v405,
  title = {{V405 Draconis: A Deep Contact Binary with a Tertiary Companion and a Quadruple System Candidate}},
  author = {Maksym Yu. Pyatnytskyy and Ivan L. Andronov},
  howpublished = {arXiv},
  year = {2026},
  month = sep,
  doi = {10.48550/arxiv.2609.35422},
  eprint = {2609.35422},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2609.35422},
  note = {CC BY 4.0},
}
RIS
TY  - UNPB
TI  - V405 Draconis: A Deep Contact Binary with a Tertiary Companion and a Quadruple System Candidate
AU  - Maksym Yu. Pyatnytskyy
AU  - Ivan L. Andronov
PY  - 2026
DA  - 2026/09/28
PB  - arXiv
DO  - 10.48550/arxiv.2609.35422
UR  - https://arxiv.org/abs/2609.35422
AB  - We continued our analysis of the O-C diagram of the EW-type eclipsing binary V405 Dra using recently available data. We refined the orbital parameters of the third body responsible for the short-period oscillations in the O-C curve, obtaining P_3=513.12(20) d, a_12sin i_3=0.3862(15) AU, and e_3=0.1690(48). Assuming a total mass of $1.56$ M_⊙ for the eclipsing binary, the minimum mass of the third body is estimated to be about $0.5$ M_⊙. We also investigated the complex long-term O-C trend and found that it may be partially explained by the light-time effect caused by a possible fourth body, with a characteristic period of about 23.5 yr and a minimum mass of about $0.9$ M_⊙. However, the fourth-body model cannot fully reproduce the observed long-term variation, particularly the earliest data, and the nature of part of the long-term trend remains unexplained.
ER  -