Catálogo de publicaciones - revistas

<jats:title>Abstract</jats:title> <jats:p>We report results of the first reverberation mapping campaign of I Zwicky 1 during 2014–2016, which showed unambiguous reverberations of the broad H<jats:italic>β</jats:italic> line emission in the varying optical continuum. From analysis using several methods, we obtain a reverberation lag of <jats:inline-formula> <jats:tex-math> <?CDATA ${\tau }_{{\rm{H}}\beta }={37.2}_{-4.9}^{+4.5}\,\mathrm{days}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab16efieqn1.gif" xlink:type="simple" /> </jats:inline-formula>. Taking a virial factor of <jats:inline-formula> <jats:tex-math> <?CDATA ${f}_{{}_{\mathrm{BLR}}}=1$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab16efieqn2.gif" xlink:type="simple" /> </jats:inline-formula>, we find a black hole mass of <jats:inline-formula> <jats:tex-math> <?CDATA ${M}_{\bullet }={9.30}_{-1.38}^{+1.26}\times {10}^{6}{M}_{\odot }$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab16efieqn3.gif" xlink:type="simple" /> </jats:inline-formula> from the mean spectra. The accretion rate is estimated to be <jats:inline-formula> <jats:tex-math> <?CDATA ${203.9}_{-65.8}^{+61.0}\,{L}_{\mathrm{Edd}}{c}^{-2}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab16efieqn4.gif" xlink:type="simple" /> </jats:inline-formula>, suggesting a super-Eddington accretor, where <jats:italic>L</jats:italic> <jats:sub>Edd</jats:sub> is the Eddington luminosity and <jats:italic>c</jats:italic> is the speed of light. By decomposing <jats:italic>Hubble Space Telescope</jats:italic> images, we find that the stellar mass of the bulge of its host galaxy is <jats:inline-formula> <jats:tex-math> <?CDATA $\mathrm{log}({M}_{\mathrm{bulge}}/{M}_{\odot })=10.92\pm 0.07$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab16efieqn5.gif" xlink:type="simple" /> </jats:inline-formula>. This leads to a black hole to bulge mass ratio of ∼10<jats:sup>−4</jats:sup>, which is significantly smaller than that of classical bulges and elliptical galaxies. After subtracting the host contamination from the observed luminosity, we find that I Zw 1 follows the empirical <jats:inline-formula> <jats:tex-math> <?CDATA ${R}_{\mathrm{BLR}}\propto {L}_{5100}^{1/2}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjab16efieqn6.gif" xlink:type="simple" /> </jats:inline-formula> relation.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Alfvénic waves have gained renewed interest since the existence of ubiquitous propagating kink waves were discovered in the corona. It has long been suggested that Alfvénic waves play an important role in coronal heating and the acceleration of the solar wind. To this effect, it is imperative to understand the mechanisms that enable their energy to be transferred to the plasma. Mode conversion via resonant absorption is believed to be one of the main mechanisms for kink wave damping and it is considered to play a key role in the process of energy transfer. This study examines the damping of propagating kink waves in quiescent coronal loops using the Coronal Multi-channel Polarimeter. A coherence-based method is used to track the Doppler velocity signal of the waves, which enables us to investigate the spatial evolution of velocity perturbations. The power ratio of outward to inward propagating waves is used to estimate the associated damping lengths and quality factors. To enable accurate estimates of these quantities, we provide the first derivation of a likelihood function suitable for fitting models to the ratio of two power spectra obtained from discrete Fourier transforms. Maximum likelihood estimation is used to fit an exponential damping model to the observed variation in power ratio as a function of frequency. We confirm earlier indications that propagating kink waves are undergoing frequency-dependent damping. Additionally, we find that the rate of damping decreases, or equivalently the damping length increases, for  longer coronal loops that reach higher in the corona.</jats:p>