Velocity-imaging the rapidly precessing planetary disc around the white dwarf HE 1349–2305 using Doppler tomography

Author:

Manser Christopher J12ORCID,Dennihy Erik3,Gänsicke Boris T24ORCID,Debes John H5,Gentile Fusillo Nicola P6ORCID,Hermes J J7,Hollands Mark2ORCID,Izquierdo Paula89,Kaiser B C10,Marsh T R2,Reding Joshua S10,Rodríguez-Gil Pablo89,Veras Dimitri24ORCID,Wilson David J11ORCID

Affiliation:

1. Astrophysics Group, Department of Physics, Imperial College London, Prince Consort Road, London, SW7 2AZ, UK

2. Department of Physics, University of Warwick, Coventry CV4 7AL, UK

3. Gemini Observatory/NSF’s NOIRLab, Casilla 603, La Serena, Chile

4. Centre for Exoplanets and Habitability, University of Warwick, Coventry CV4 7AL, UK

5. AURA for ESA, Space Telescope Science Institute, Baltimore, MD, USA

6. European Southern Observatory, Karl-Schwarzschild-Street 2, Garching D-85748, Germany

7. Department of Astronomy, Boston University, Boston, MA 02215, USA

8. Instituto de Astrofísica de Canarias, La Laguna E-38205, Tenerife, Spain

9. Departamento de Astrofísica, Universidad de La Laguna, La Laguna E-38206, Tenerife, Spain

10. Department of Physics and Astronomy, University of North Carolina at Chapel Hill, Chapel Hill, NC 27599, USA

11. McDonald Observatory, University of Texas at Austin, Austin, TX 78712, USA

Abstract

ABSTRACT The presence of planetary material in white dwarf atmospheres, thought to be accreted from a dusty debris disc produced via the tidal disruption of a planetesimal, is common. Approximately 5 per cent of these discs host a co-orbital gaseous component detectable via emission from atomic transitions  –  usually the 8600 Å Ca ii triplet. These emission profiles can be highly variable in both morphology and strength. Furthermore, the morphological variations in a few systems have been shown to be periodic, likely produced by an apsidally precessing asymmetric disc. Of the known gaseous debris discs, that around HE 1349–2305 has the most rapidly evolving emission-line morphology, and we present updated spectroscopy of the Ca ii triplet of this system. The additional observations show that the emission-line morphologies vary periodically and consistently, and we constrain the period to two aliases of 459 ± 3 and 502 ± 3 d. We produce images of the Ca ii triplet emission from the disc in velocity space using Doppler tomography  –  only the second such imaging of a white dwarf debris disc. We suggest that the asymmetric nature of these velocity images is generated by gas moving on eccentric orbits with radially dependent excitation conditions via photoionization from the white dwarf. We also obtained short-cadence (≃4 min) spectroscopy to search for variability on the time-scale of the disc’s orbital period (≃hours) due to the presence of a planetesimal, and rule out variability at a level of ≃1.4 per cent.

Funder

STFC

Imperial College London

Leverhulme Trust

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

Cited by 2 articles. 订阅此论文施引文献 订阅此论文施引文献,注册后可以免费订阅5篇论文的施引文献,订阅后可以查看论文全部施引文献

1. Planetesimals drifting through dusty and gaseous white dwarf debris discs: Types I, II and III-like migration;Monthly Notices of the Royal Astronomical Society;2023-06-14

2. A DZ white dwarf with a 30 MG magnetic field;Monthly Notices of the Royal Astronomical Society;2023-01-14

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