Wide binary stars are used to test the modified gravity called Scalar-Tensor-Vector Gravity or MOG. This theory is based on the additional gravitational degrees of freedom, the scalar field G=GN(1+α), where GN is Newton's constant, and the massive (spin-1 graviton) vector field ϕμ. The wide binaries have separations of 2-30 kAU. The MOG acceleration law, derived from the MOG field equations and equations of motion of a massive test particle for weak gravitational fields, depends on the enhanced gravitational constant G=GN(1+α) and the effective running mass μ. The magnitude of α depends on the physical length scale or averaging scale ℓ of the system. The modified MOG acceleration law for weak gravitational fields predicts that for the solar system and for the wide binary star systems gravitational dynamics follows Newton's law.
Thursday, November 30, 2023
Wide Binaries Are Basically Newtonian in Moffat's MOG Theory
Monday, November 20, 2023
A Newly Discovered Milky Way Satellite Star Cluster
Wednesday, November 15, 2023
Are Sunspots Driven By The Gravitational Pull Of The Planets?
The sunspot number record covers over three centuries.These numbers measure the activity of the Sun. This activity follows the solar cycle of about eleven years.
In the dynamo-theory, the interaction between differential rotation and convection produces the solar magnetic field. On the surface of Sun, this field concentrates to the sunspots. The dynamo-theory predicts that the period, the amplitude and the phase of the solar cycle are stochastic.
Here we show that the solar cycle is deterministic, and connected to the orbital motions of the Earth and Jupiter. This planetary-influence theory allows us to model the whole sunspot record, as well as the near past and the near future of sunspot numbers. We may never be able to predict the exact times of exceptionally strong solar flares, like the catastrophic Carrington event in September 1859, but we can estimate when such events are more probable. Our results also indicate that during the next decades the Sun will no longer help us to cope with the climate change. The inability to find predictability in some phenomenon does not prove that this phenomenon itself is stochastic.
Friday, November 10, 2023
A Nifty New Telescope
Nestled in the mountains of Northern India, is a 4-metre rotating dish of liquid mercury. Over a 10-year period, the International Liquid Mirror Telescope (ILMT) will survey 117 square degrees of sky, to study the astrometric and photometric variability of all detected objects. . . .
A perfect reflective paraboloid represents the ideal reference surface for an optical device to focus a beam of parallel light rays to a single point. This is how astronomical mirrors form images of distant stars in their focal plane. In this context, it is amazing that the surface of a liquid rotating around a vertical axis takes the shape of a paraboloid under the constant pull of gravity and centrifugal acceleration, the latter growing stronger at distances further from the central axis. The parabolic surface occurs because a liquid always sets its surface perpendicular to the net acceleration it experiences, which in this case is increasingly tilted and enhanced with distance from the central axis. The focal length F is proportional to the gravity acceleration g and inversely proportional to the square of the angular velocity ω. In the case of the ILMT, the angular velocity ω is about 8 turns per minute, resulting in a focal length of about 8m. Given the action of the optical corrector, the effective focal length f of the D=4m telescope is about 9.44m, resulting in the widely open ratio f/D∼2.4. In the case of the ILMT, a thin rotating layer of mercury naturally focuses the light from a distant star at its focal point located at ∼8m just above the mirror, with the natural constraint that such a telescope always observes at the zenith.Thanks to the rotation of the Earth, the telescope scans a strip of sky centred at a declination equal to the latitude of the observatory (+29◦21′41.4′′ for the ARIES Devasthal observatory). The angular width of the strip is about 22′, a size limited by that of the detector (4k×4k) used in the focal plane of the telescope. Since the ILMT observes the same region of the sky night after night, it is possible either to co-add the images taken on different nights in order to improve the limiting magnitude or to subtract images taken on different nights to make a variability study of the corresponding strip of sky. Consequently, the ILMT is very well-suited to perform variability studies of the strip of sky it observes. While the ILMT mirror is rotating, the linear speed at its rim is about 5.6km/hr, i.e., the speed of a walking person.
A liquid mirror naturally flows to the precise shape paraboloid shape needed because it is a liquid under these conditions. And, since its surface is always dynamically readjusting itself to this shape, rather than being fixed in place just once as a solid mirror would be, any slight imperfections in its surface that do deviate from its paraboloid shape don't stay in exactly the same place. Instead, distortions from slight imperfections in the shape of the liquid mirror average out over multiple observations of the same part of the sky, to an average shape at any one location that is much closer to perfect than a solid mirror cast ultra-precisely just once. Thus, a liquid mirror reduces one subtle source of potential systemic errors that can arise from slight imperfections in the mirror's shape at particular locations that recur every time a particular part of the sky is viewed when a solid mirror is used.
A New Top Quark Pole Mass Analysis And A Few Wild Conjectures Considered
A new paper makes an re-analysis of existing data to determine the top quark pole mass. It comes up with:
which is consistent with, but at the low end of the range of the Particle Data Group's estimate based upon indirect cross-section measurements (bringing these into the same amount of precision as its direct measurements of the top quark mass):
The global LC&P relationship (i.e. that the sum of the squares of the fundamental SM particle masses is equal to the square of the Higgs vev, which is equivalent to saying that the sum of the SM particle Yukawas is exactly 1), which is about 0.5% less than the predicted value (2 sigma in top quark and Higgs boson mass, implying a theoretically expected top quark mass of 173,360 MeV and a theoretically expected Higgs boson mass of 125,590 MeV if the adjustments were proportioned to the experimental uncertainty in the LC&P relationship given the current global average measurements, in which about 70% of the uncertainty is from the top quark mass uncertainty and about 29% is from the Higgs boson mass uncertainty). . . .But, the LC&P relationship does not hold separately for fermions and bosons, which would be analogous in some ways to supersymmetry. This is only an approximate symmetry. The sum of the squares of the SM fundamental boson masses is more than half of the square of the Higgs vev by about 0.5% (3.5 sigma of Higgs boson mass, implying a theoretically expected Higgs boson mass of about 124,650 MeV), while the sum of the squares of the SM fundamental fermion masses is less than half of the square of the Higgs vev by about 1.5% (about 2.8 sigma of top quark mass, implying a theoretically expected top quark mass of about 173,610 MeV). The combined deviation from the LC&P relationship for both fermions and bosons independently is 4.5 sigma, which is a very strong tensions that is nearly conclusively ruled out. One wonders if the slightly bosonic leaning deviation from this symmetry between fundamental fermion masses and fundamental boson masses has some deeper meaning or source.
The result in this new paper, by largely corroborating direct measurements of the top quark mass at similar levels of precision, continues to favor a lower top quark mass than the one favored by LP&C expectations.
Earlier, lower energy Tevatron measurements of the top quark mass (where the top quark was discovered) supported higher values for the top quark mass than the combined data from either of the Large Hadron Collider (LHC) experiments do and was closely in line with the LP&C expectation.
But there is no good reason to think that both of the LHC experiments measuring the top quark mass have greatly understated the systemic uncertainties in their measurements (which combine measurements from multiple channels with overlapping but not identical sources of systemic uncertainty). Certainly, the LHC experiments have much larger numbers of top quark events to work with than the two Tevatron experiments measuring the top quark mass did, so the relatively low statistical uncertainties of the LHC measurements of the top quark mass are undeniably something that makes their measurements more precise relative to Tevatron.
Could This Hint At Missing Fundamental Particles?
If I were a phenomenologist prone to proposing new particles, I'd say that this close but not quite right fit to the LP&C hypothesis was a theoretical hint that the Standard Model might be missing one or more fundamental particles, probably fermions (which deviate most strongly from the expected values).
I'll explore some of those possibilities, because readers might find them to be interesting. But, to be clear, I am not prone to proposing new particles, indeed, my inclinations are quite the opposite. I don't actually think that any of these proposals is very well motivated.
In part, this is because I think that dark matter phenomena and dark energy phenomena are very likely to be gravitational issues rather than due to dark matter particles or dark energy bosonic scalar fields, I don't think we need need particles to serve that purpose. Dark matter phenomena would otherwise be the strong motivator for a beyond the Standard Model new fundamental particle.
I am being lenient in not pressing some of the more involved arguments from the data and theoretical structure of fundamental physics that argue against the existence of many of these proposed beyond the Standard Model fundamental particles.
This is so, even though the LP&C hypothesis is beautiful, plausible, and quite close to the experimental data, so it would be great to be able to salvage it somehow if the top quark mass and Higgs boson mass end up being close to or lower than their current best fit estimated values.
Beyond The Standard Model Fundamental Fermion Candidates
If the missing fermion were a singlet, LP&C would imply an upper bound on its mass of about 3 GeV.
This could be a good fit for a singlet sterile neutrino that gets its mass via the Higgs mechanism and then transfers its own mass to the three active neutrinos via a see-saw mechanism.
It could also be a good fit for a singlet spin-3/2 gravitino in a supersymmetry inspired model in which only the graviton, and not the ordinary Standard Model fermions and bosons have superpartners.
A largely sterile singlet gravitino, and a singlet sterile neutrino, have both been proposed as cold dark matter candidates and at masses under 3 GeV the bounds on their cross-sections of interaction (so that they could have some self-interaction or weak to feeble interaction with ordinary matter since purely sterile dark matter that only interacts via gravity isn't a good fit for the astronomy data) aren't as tightly constrained as heavier WIMP candidates. And, the constraints on a WIMP dark matter particle cross section of interaction from direct dark matter detection experiments gets even weaker fairly rapidly between 3 GeV and 1 GeV, which is what the LP&C conjecture would hint at if either the current best fit value for the top quark mass or the current best fit value for the Higgs boson mass were a bit light.
The LP&C conjecture isn't a useful hint towards (or against) a massive graviton, however, because the experimental bounds on those are on the order of 32 orders of magnitude or more too small to be discernible by that means.
If there were three generations of missing fermions, you'd expect them to have masses about two-thirds higher than the charged lepton masses, with the most massive one still close to 3 GeV, the second generation one at about 176 MeV, and the first generation one at about 0.8 MeV. But these masses could be smaller if the best fit values for the top quark mass and/or Higgs boson mass ended rising somewhat as the uncertainties in those measurements fall.
These masses for a missing fermion triplet might fit a leptoquark model of the kind that has been proposed to explain B meson decay anomalies. The experimental motivation for leptoquarks was stronger before the experimental data supporting violations of the Standard Model principle of charged lepton universality (i.e. that the three charged leptons have precisely the same properties except their masses) evaporated in the face of factors in the data analysis of the seemingly anomalous experimental results from B meson decays. But there are still some lesser and subtle anomalies in B meson decays that didn't go away with this improved data analysis that could motivate similar leptoquark models.
If there were two missing fermions of similar masses (or two missing fermion triplets with their sum of square masses dominated by the third-generation particle of each triplet), this would suggest a missing fundamental particle mass on the order of up to about 2 GeV each.
A model with two missing fermion triplets might make sense if there were two columns of missing leptoquarks, instead of one, just as there are two columns of quarks (up type and down type) and two columns of leptons (charged leptons and neutrinos), in the Standard Model.
Wednesday, November 8, 2023
More On Wide Binaries, MOND and Deur
We test Milgromian dynamics (MOND) using wide binary stars (WBs) with separations of 2−30 kAU. Locally, the WB orbital velocity in MOND should exceed the Newtonian prediction by ≈20% at asymptotically large separations given the Galactic external field effect (EFE).
We investigate this with a detailed statistical analysis of Gaia DR3 data on 8611 WBs within 250 pc of the Sun. Orbits are integrated in a rigorously calculated gravitational field that directly includes the EFE. We also allow line of sight contamination and undetected close binary companions to the stars in each WB. We interpolate between the Newtonian and Milgromian predictions using the parameter αgrav, with 0 indicating Newtonian gravity and 1 indicating MOND.
Directly comparing the best Newtonian and Milgromian models reveals that Newtonian dynamics is preferred at 19σ confidence. Using a complementary Markov Chain Monte Carlo analysis, we find that αgrav=−0.021+0.065−0.045, which is fully consistent with Newtonian gravity but excludes MOND at 16σ confidence. This is in line with the similar result of Pittordis and Sutherland using a somewhat different sample selection and less thoroughly explored population model.
We show that although our best-fitting model does not fully reproduce the observations, an overwhelmingly strong preference for Newtonian gravity remains in a considerable range of variations to our analysis.
Adapting the MOND interpolating function to explain this result would cause tension with rotation curve constraints. We discuss the broader implications of our results in light of other works, concluding that MOND must be substantially modified on small scales to account for local WBs.
The immense diversity of the galaxy population in the universe is believed to stem from their disparate merging histories, stochastic star formations, and multi-scale influences of filamentary environments. Any single initial condition of the early universe was never expected to explain alone how the galaxies formed and evolved to end up possessing such various traits as they have at the present epoch. However, several observational studies have revealed that the key physical properties of the observed galaxies in the local universe appeared to be regulated by one single factor, the identity of which has been shrouded in mystery up to date.
Here, we report on our success of identifying the single regulating factor as the degree of misalignments between the initial tidal field and protogalaxy inertia momentum tensors. The spin parameters, formation epochs, stellar-to-total mass ratios, stellar ages, sizes, colors, metallicities and specific heat energies of the galaxies from the IllustrisTNG suite of hydrodynamic simulations are all found to be almost linearly and strongly dependent on this initial condition, when the differences in galaxy total mass, environmental density and shear are controlled to vanish. The cosmological predispositions, if properly identified, turns out to be much more impactful on galaxy evolution than conventionally thought.