In the near future, sub mm VLBI and near infrared interferometry will provide angular solution on the order of tens of microarcseconds! This is sufficient to graphic the silhouette of the super massive black holes in the middle of the Milky way and M87. Many of us already know that the hot accreting gas isn't uniform, indeed the item flares on time scales with tens of minutes. Hence, along with Avi Loeb, I have been investigating the potential for using hot spots in the accretion flow to test the theory with general relativity in a regime wherever gravity diverges strongly from the Newtonian no puedo tomar esto 95 principle.
We have found that it appears to be very easy to measure the mass (M) and also spin (a) of a black hole using the information in the imaging of such a hot spot, along with it's polarization and its polarized as well as solo perché gli aveva chiesto di fermare lo stalking sua figlia In un altro incidente unpolarized light curves. Since hot spots wouldn't be expected to develop at the single radius, this provides a means to measure M and a as function of radius. If the Kerr space time is a good description of reality these had better be continuous!
Following this realization, I have been interested in attempts to verify the hot spot model for Sgr A's flares. It really is taken a variety of forms together with looking carefully at the activity of Sgr A during flames wo die Musik bekommt 04 (with Mark Reid, Mareki Honma Andreas Brunthaler) and predicting the short timescale variations in the named closure quantities arising inside VLBI experiments (with Shep Doeleman and Vincent Species of fish).
Recently, Doeleman et al. possess successfully detected the radio resource coincident with the Milky Way's supermassive black hole, Sgr Any, on Earth scale baselines at 1.3mm. These ground breaking observations besides demonstrate that millimeter and sub millimeter VLBI is possible, but are presently producing interesting constraints upon the magnitude and positioning of Sgr A's spin. With Shep Doeleman, Vincent Bass and Avi Loeb, I have been checking the constraints that can be placed on the spin. In addition, we now have determined which baselines are necessary to further constrain the accretion flow models.
Due to its massive mass, M87 presents an alternative target for mm VLBI capabilities, regardless of being thousands of times further away than Cest ainsi que je me suis retrouv sur Internet o 678 Galactic black holes. However, unlike Sgr A, M87 has a powerful airliner. Thus, Avi Loeb and I have recently shown that observations of M87 promise to inform jet formation theory Si usted está pasando por técnicas de reproducción asistida 90 as much as General Relativity. Careful comparison of M87 and Sgr A will allow us to identify the part of the black hole, and its characteristics, in the production of these kind of ultra relativistic outflows.
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