Bow shock nebulae of hot massive stars in a magnetized medium

摘要: A significant fraction of OB-type, main-sequence massive stars are classified as runaway and move supersonically through the interstellar medium (ISM). Their strong stellar winds interact with their surroundings where typical strength local ISM magnetic field is about 3.5-7 micro-G, which can result in formation bow shock nebulae. We investigate effects such fields, aligned motion flow, on emission properties these circumstellar structures. Our axisymmetric, magneto-hydrodynamical simulations optically-thin radiative cooling, heating anisotropic thermal conduction show that presence background affects projected optical our shocks at Ha [OIII] lambda 5007 become fainter by 1-2 orders magnitude, respectively. Radiative transfer calculations against dust opacity indicate slightly diminishes infrared emit brightly 60 micron. This may explain why generated ionizing often difficult to identify. Finally, we discuss results context Zeta Ophiuchi support interpretation its imperfect morphology an evidence not driving star.