Secondary Accceleration of Cosmic Rays by Supernova Shocks

In the common model supernova shock-acceleration of cosmic rays there are two open questions: 1. where does the high energy cosmic rays below the knee (10$^4-10^6$ Gev) come from, and 2. are cosmic ray accelerated only at their origin or contineuosly during their residence in the Galaxy. We show that $10^15$ eV light nuclei are probably accelerted by associations of supernovae. The ratio of the spectra of secondary to primary cosmic rays would be affected by repeated acceleration (also called reacceleration or secondary acceleration) in the ISM during their propagation in the galaxy. The observed secondary and primary CR spectra are used to constrain the amount of such reacceleration by supernova remnants (SNR). Two cases are considered: weak shocks ($1<M<2$) of old, dispersed remnants, and strong shocks ($M>3$) of relatively young remnants. It is shown that weak shocks produce more reacceleration than what is permitted in the framework of the standard leaky box (SLB) model, making it inconsistent with dispersed acceleration that should be produced by SNR. If the SLB is modified to allow a moderate amount of RA by week shocks, the RA produced by old SNRs agrees with the rate required to fit the secondary-to primaray cosmic-ray data, making a self consistent picture. Significant reacceleration by strong shocks of young SNRs should lead to flattening of the secondary-to primaray ratio at high energies, near 1TeV/nucleon.Comment: 4 page latex file. Complete uuencoded compressed PS file is also available at ftp://saba.fiz.huji.ac.il/pub/wandel/cr_icrc.uu or at http://shum.cc.huji.ac.il/~amri/papers/cr_icrc(tex,ps) In the procceeding of the 25th ICRC, v.4 p.41

Black Holes and Hosts of Active and Quiescent Galaxies: I. The Black Hole-Bulge Relation revisited

Massive Black Holes detected in the centers of many nearby galaxies show an approximately linear relation with the luminosity of the host bulge, with the black hole mass being 0.001-0.002 of the bulge mass. Previous work suggested that black holes of active (Seyfert 1) galaxies follow a similar relation, but apparently with a significantly lower value of $M_{\rm BH}/M_{\rm bulge}$ (Wandel 1999). New data show that this difference was mainly due to overestimating the black hole mass in quiescent galaxies and overestimating the bulge magnitude of Seyfert galaxies. Using new and updated data we show that AGNs (Seyfert galaxies and quasars) follow the same BH-bulge relation as ordinary (inactive) galaxies. We derive the BH-bulge relation for a sample of 55 AGNs and 35 quiescent galaxies, finding that broad line AGNs have an average black hole/bulge mass fraction of $\sim 0.0015$ with a strong correlation (Mbh ~ Lbulge^{0.9\pm 0.16}). This BH-bulge relation is consistent with the BH-bulge relation of quiescent galaxies and much tighter than previous results. Narrow line AGNs appear to have a lower ratio, Mbh/Mbulge ~ 10^{-4}-10^{-3}. We find this to be a more general feature, the BH/bulge ratio in AGNs being inversely correlated with the emission-line width, implying a strong linear relation between the size of the broad emission line region and the luminosity of the bulge. Finally, combining AGNs with observed and estimated stellar velocity dispersion, we find a significant correlation (Mbh ~ v^{3.5-5}), consistent with that of quiescent galaxies.Comment: 11 pages, 7 figures, accepted for publication in the Astrophysical Journal, submitted July 1

Evolutionary Baldwin Effect in AGN

Assuming Active Galactic Nuclei are powered by accretion onto a massive black holes we suggest that the growth of the central black hole due to the matter accreted over the AGN lifetime causes an evolution of the luminosity and spectrum. We show that the effective temperature of the UV continuum spectrum is likely to be anti-correlated with the black-hole mass and with the accretion-powered luminosity. We estimate the change in the equivalent width of the emission lines due to the growth of the black hole and show that for plausible evolutionary tracks and effective-temperature models the equivalent width is anti-correlated with continuum luminosity thus implying an evolutionary origin to the Baldwin effect.Comment: 12 pages LaTeX, 1 enclosed figure. To appear in the proceedings of "Quasars as Standard Candles for Cosmology" (May 18-22, 1998, La Serena, Chile), to be published by ASP, ed. G. Ferlan

Riesz transform for Dunkl Hermite expansion

In the present paper, we establish that Riesz transforms for Dunkl Hermite expansion as introduced in [4] are singular integral operators with H\"ormander's type conditions and we show that are bounded on $L^p(\mathbb{R}^d; d\mu_k) 1 < p < 1.Comment: 13 page

On the BH-galaxy relation of AGN and Narrow Line Seyfert 1 Galaxies

Massive black holes (BHs) are detected in the centers of many nearby galaxies are linearly correlated with the luminosity of the host bulge (spheroid), the black hole mass being about 0.1% of the stellar mass. In active galaxies, the BH mass is best measured by the reverberation mapping (light echo) technique. We and others have shown that in AGNs the BH mass follows the same relation with the luminosity of the host galaxy as in ordinary (inactive) galaxies, with the exception of narrow line AGNs which apparently have significantly lower values of the BH/bulge mass (or BH/bulge luminosity) ratio. The BH/bulge ratio is also found to be strongly correlated with the velocity dispersion of the broad line-emitting gas in the active nucleus. However, in the BH-stellar velocity relation the difference between broad- and narrow-line AGNs (in particular NLS1s) seems to be less obvious. We review the subject adding recent updates and suggestions.Comment: 9 pages, 6 figures, Narrow-Line Seyfert 1 Galaxies and Their Place in the Universe (NLS1 Milan, Italy

On the integral representations for Dunkl kernels of type A2A_{2}

We give an explicit integral formula for the Dunkl kernel associated to root system of type $A_2$ and parameter $k>0$, by exploiting recent result in [1]

Quantum Behavior of Measurement Apparatus

We precise for the first time the quantum behavior of a measurement apparatus in the framework of the usual interpretation of quantum physics. We show how such a behavior can also be studied by the retrodiction of pre-measurement states corresponding to its responses. We translate in terms of these states some interesting properties of the behavior of an apparatus, such as the projectivity, the fidelity, the non-Gaussian character, or the non-classicality of measurements performed by this one. We also propose an experimental procedure allowing the tomography of these pre-measurement states for optical detectors. We illustrate the relevance of these new notions for measurements, by evaluating them for two detectors widely used in quantum optics: the avalanche photodiode and the homodyne detection.Comment: APS Preprint format : 19 pages with 6 figures, a new figure (Fig. 2) was added. Questions and comments are welcom

On the bio-habitability of M-dwarf planets

The recent detection of Earth-sized planets in the habitable zone of Proxima Centauri, Trappist-1 and many other nearby M-type stars has led to speculations, whether liquid water and life actually exist on these planets. To a large extent, the answer depends on their yet unknown atmospheres, which may though be within observational reach in the near future by JWST, ELT and other planned telescopes. We consider the habitability of planets of M-type stars in the context of their atmospheric properties, heat transport and irradiation. Instead of the traditional definition of the habitable zone, we define the bio-habitable zone, where liquid water and complex organic molecules can survive on at least part of the planetary surface. The atmospheric impact on the temperature is quantified in terms of the heating factor (a combination of greenhouse heating, stellar irradiation, albedo etc.) and heat redistribution (horizontal energy transport). We investigate the bio-habitable domain (where planets can support surface liquid water and organics) in terms of these two factors. Our results suggest that planets orbiting M-type stars may have life-supporting temperatures, at least on part of their surface, for a wide range of atmospheric properties. We apply this analyses to Proxima b and the Trappist-1 system. Finally we discuss the implications to the search of biosignatures and demonstrate how they may be used to estimate the abundance of photosynthesis and biotic planets.Comment: 33 pages, 15 figure

The Mass-Luminosity Relation in AGN

Probably the most fundamental characteristic of the quasar-AGN power house, the mass of the central black hole, is the least well known. I review the three main classes of mass estimation methods---broad emission-line kinematics, X-ray variability and accretion-disk modeling, and the masses they give in terms of the Eddington ratio, $L/L_{\rm Edd}$. The broad emission lines are probably the best probe of the central mass. They provide mass estimates that suggest a narrow spread for the Eddington ratio - 1--2 orders of magnitude over more than six orders of magnitude in continuum luminosity, possibly indicating a universal $M/L$ ratio for AGN. However, other methods give a larger spread and possibly a luminosity- dependent Eddington ratio. Potential sources of errors and bias are discussed.Comment: 13 pages, Latex (aspconf.sty), 4 postscript figures. Also available at http://shum.cc.huji.ac.il/~amri/papers/ml Review to appear in procs. of "Structure and Kinematics of Quasar Broad Line Regions" (23-26 March 1998, Lincoln, Nebraska) eds. Gaskell, C. M., Brandt, W. N., Dietrich, M., Dultzin-Hacyan, D. & Eracleous, M. (ASP Press: San Francisco

Spectral Dependence of the Broad Emission-Line Region in AGN

We derive a theoretical relation between $R_{BLR}$, the size of the broad-emission-line region of active galactic nuclei, and the observed soft X-ray luminosity and spectrum. We show that in addition to the well known $R_{BLR}\sim L^{1/2}$ scaling, $R_{BLR}$ should depend also on the soft X-ray spectral slope and derive the expected relation between $R_{BLR}$ and the X-ray luminosity and spectral index. Applying this relation to calculate a predicted BLR radius for ten AGN with reverberation data, we show that including the dependence on the spectrum improves the agreement between the calculated BLR radius and the radius independently determined from reverberation mapping. Similarly, we evaluate an expression for the line width, and show that including the dependence on the spectrum significantly improves the agreement between the calculated BLR velocity dispersion and the observed FWHM of the H$\beta$ line.Comment: 8 pages, Latex (aas2pp4.sty), 5 postscript figures. Also available at http://shum.cc.huji.ac.il/~amri/papers/blr Accepted for publication in the Astrophysical Journal Letter