
WEIGHT: 60 kg
Bust: DD
1 HOUR:140$
Overnight: +90$
Services: Massage, Golden shower (out), Golden shower (in), BDSM, Mistress
Massive stars are recognized for their high degree of multiplicity, yet the mass ratio regime below 0. It is therefore unknown whether extremely low-mass possibly substellar companions can form and survive in the direct UV-irradiated environment of massive stars. Two targets have companions that are brown dwarf candidates. For three of these, we have obtained a second epoch observation. At least two sources exhibit similar proper motion to that of their central star.
However, given the expected proper motion of background objects, this does not imply certain companionship. The vast majority of massive stars are found in binaries and multiple systems Mason et al. For low-mass stars, this mechanism is expected to create companions at relatively close initial separations 10 - AU, Offner et al. Observational constraints on the multiplicity properties of massive stars are of crucial importance in order to understand their formation.
However, the mass ratio regime below 0. For spectroscopic binaries, mass ratios close to 0. Recently, high-contrast imaging has been proven to be well-suited to find extremely low mass-ratio companions at intermediate and wide separations. So far, the study has proven to be successful with the discovery of a It is unclear how these substellar objects could have been formed and survived around massive stars, since their strong UV radiation creates a harsh environment for such low-mass objects to be formed Armitage, ; Nicholson et al.
For this reason, it has been proposed that substellar companions might have been created through capture free-floating object or theft steal a companion from another star. The number of companions peaks around an age of 0. However, it remains uncertain whether these candidate companions are truly bound or whether they are spurious associations that arize due to line-of-sight alignment. Confirming that some of these companions are bound through follow-up observations is challenging because OB stars are typically located in distant star-forming regions and OB associations.
Consequently, OB stars exhibit small proper motion and parallax. Despite these difficulties, it is crucial to attempt to confirm that some of the low-mass candidate companions are indeed gravitationally bound to their central massive star. These systems have mass ratios between 0.