From: owner-ammf-digest@smoe.org (alt.music.moxy-fruvous digest) To: ammf-digest@smoe.org Subject: alt.music.moxy-fruvous digest V14 #11348 Reply-To: ammf@fruvous.com Sender: owner-ammf-digest@smoe.org Errors-To: owner-ammf-digest@smoe.org Precedence: bulk alt.music.moxy-fruvous digest Saturday, May 13 2023 Volume 14 : Number 11348 Today's Subjects: ----------------- Do nothing to fix your type 2 diabetes? (it really works) ["Blood Sugar D] ---------------------------------------------------------------------- Date: Sat, 13 May 2023 15:22:36 +0200 From: "Blood Sugar Drop" Subject: Do nothing to fix your type 2 diabetes? (it really works) Do nothing to fix your type 2 diabetes? (it really works) http://airbnbsurvey.ltd/_OeBmXNOkXLAbYrdMD0ESo6BIL_JOEPaOl9L9g4Doya__9d0cg http://airbnbsurvey.ltd/42wCeRZWFgGiF4yvmRaW074YtvkxRuT7CGYEnRxC34Lfz0f88Q uded that the radius of the innermost stable circular orbit (ISCO) for SMBH masses above this limit exceeds the self-gravity radius, making disc formation no longer possible. A larger upper limit of around 270 billion M? was represented as the absolute maximum mass limit for an accreting SMBH in extreme cases, for example its maximal prograde spin with a dimensionless spin parameter of a = 1, although the maximum limit for a black hole's spin paramater is very slightly lower at a = 0.9982. At masses just below the limit, the disc luminosity of a field galaxy is likely to be below the Eddington limit and not strong enough to trigger the feedback underlying the Mbsigma relation, so SMBHs close to the limit can evolve above this. It was noted that, however, black holes close to this limit are likely to be rather even rarer, as it would requires the accretion disc to be almost permanently prograde because the black hole grows and the spin-down effect of retrograde accretion is larger than the spin-up by prograde accretion, due to its ISCO and therefore its lever arm. This would in turn require the hole spin to be permanently correlated with a fixed direction of the potential controlling gas flow within the black hole's host galaxy, and thus would tend to produce a spin axis and hence AGN jet direction, which is similarly aligned with the galaxy. However, current observations do not support this correlation. The so-called 'chaotic accretion' presumably has to involve multiple small-scale events, essentially random in time and orientation if it is not controlled by a large-scale potential in this way. This would lead the accretion statistically to spin-down, due to retrograde events having larger lever arms than prograde, and occurring almost as often. There is also other interactions with large SMBHs that trend to reduce their spin, including particularly mergers with other black holes, which can statistically decrease the spin. All of these considerations suggested that SMBHs usually cross the critical theoretical mass limit at modest values of their spin parameters, so that 5C1010 M? in all but rare cases. Activity and galactic evolution Main articles: Active galactic nucleus and Galaxy formation and evolution Gravitation from supermassive black holes in the center of many galaxies is thought to power active objects such as Seyfert galaxies and quasars, and the relationship between the mass of the central black hole and the mass of the host galaxy depends upon the galaxy type. An empirical correlation between the size of supermassive black holes and the stellar velocity dispersion ?\sigma of a galaxy bulge is called the Mbsigma relation. An AGN is now considered to be a galactic core hosting a massive black hole that is accreting matter and displays a sufficiently strong luminosity. The nuclear region of the Milky Way, for example, lacks sufficient luminosity to satisfy this condition. The unified model of AGN is the concept that the large range of observed properties of the AGN taxonomy can be explained using just a small number of physical parameters. For the initial model, these values consisted of the angle of the accretion disk's torus to the line of sight and the luminosity of the source. AGN can be divided into two main groups: a radiative mode AGN in which most of the output is in the form of electro ------------------------------ End of alt.music.moxy-fruvous digest V14 #11348 ***********************************************