Dense molecular globulettes and the dust arc toward the runaway O star AE Aurigae (HD 34078)^⋆,⋆⋆

¹ IRAM, 300 rue de la Piscine, 38406 Saint-Martin d’ Hères France
e-mail: gratier@iram.fr, pety@iram.fr
² Univ. Bordeaux, LAB, UMR 5804, 33270 Floirac, France
³ CNRS, LAB, UMR 5804, 33270 Floirac, France
⁴ LERMA, UMR 8112, CNRS, Observatoire de Paris, ENS, UPMC, UCP, 61 avenue de l’Observatoire, 75014 Paris, France
⁵ IAP, UMR 7095 CNRS and Sorbonne Universités, UPMC Univ Paris 06, 98bis boulevard Arago, 75014 Paris, France
⁶ VATLY, Institute for Nuclear Science and Technology, 179 Hoang Quoc Viet, Cau Giay, Ha Noi, Viet Nam
⁷ IAS, UMR 8617, CNRS, Bâtiment 121, Université Paris Sud 11, 91405 Orsay, France

Received: 19 January 2014
Accepted: 25 March 2014

Abstract

Context. Some runaway stars are known to display IR arc-like structures around them, resulting from their interaction with surrounding interstellar material. The properties of these features as well as the processes involved in their formation are still poorly understood.

Aims.We aim to understand the physical mechanisms that shape the dust arc observed near the runaway O-star AE Aur (HD 34078).

Methods.We obtained and analyzed a high spatial resolution (4.4′′) map of the ¹²CO(1−0) emission that is centered on HD 34078, and that combines data from both the IRAM interferometer and 30 m single-dish antenna.

Results. One third of the 30 m flux mainly originates from two small (no larger than 5′′ × 10′′ or 0.013 × 0.026 pc), and bright (1 and 3 K peak temperatures) CO globulettes. The line of sight toward HD 34078 intersects the outer part of one of the globulettes, which accounts for both the properties of diffuse UV light observed in the field and the numerous molecular absorption lines detected in HD 34078’s spectra, including those from highly excited H₂. Their modeled distance from the star(0.2 pc) is compatible with the fact that they lie on the 3D paraboloid, which fits the arc detected in the 24 μm Spitzer image. Four other compact CO globulettes are detected in the mapped area, all lying close to the rim of this paraboloid. These globulettes have a high density and linewidth, and are strongly pressure-confined or transient.

Conclusions. The presence of molecular globulettes at such a close distance from an O star is unexpected, and probably related to the high proper motion of HD 34078. Indeed, the good spatial correlation between the CO globulettes and the IR arc suggests that they result from the interaction of the radiation and wind emitted by HD 34078 with the ambient gas. However, the details of this interaction remain unclear. A wind mass-loss rate significantly larger than the value inferred from UV lines is favored by the large IR arc size, but does not easily explain the low velocity of the CO globulettes. The effect of radiation pressure on dust grains also meets several issues in explaining the observations. Further observational and theoretical work is needed to fully elucidate the processes shaping the gas and dust in bow shocks around runaway O stars.