arXiv subjects

T. Hosokawa

Publications and source records attributed to T. Hosokawa.

14 recordsLinked to original sources

arXiv2026

Thermochemical constraints on a primordial-origin of gas-rich debris disks

Recent observations have revealed gas-rich debris disks around intermediate-mass stars at ages of tens of Myr. The origin of this gas remains unclear: it may be primordial, retained from the protoplanetary phase, or secondary, released from volatile-rich solids. Secondary-origin models reproduce CO emission but often overpredict neutral carbon. Recent observations and disk-evolution models suggest that primordial gas may survive longer than previously assumed, motivating thermochemical tests of the primordial-remnant scenario. We test the previously unexplored possibility that primordial-origin disks satisfy the observational constraints on gas-rich debris disks. Specifically, we determine under what conditions a disk around a $2\,M_{\odot}$ star reproduces substantial CO, low CI/CO ratios, and weak HCO+ emission consistent with current non-detections. We post-processed 20-40 Myr structures from 1D disk-evolution models with Cloudy, varying irradiation geometry, dust-to-gas mass ratio (DTG), and cosmic-ray ionisation rate. In the dust-poor models (DTG $=10^{-4}$), CO remains optically thick around $R\sim100$~au. The models yield low disk-integrated CI/CO mass ratios. Our model produces CO radial intensities of the observed order of magnitude, but its CI-emitting region is more extended than observed. The standard CR model overproduces HCO+, whereas the weak CR model brings its predicted luminosity within current observational limits. These results demonstrate that a primordial origin remains chemically viable for CO-rich debris disks. The main remaining tension is the excessive radial extent of the CI emission, although it may reflect our simplified modelling. Further testing of the primordial-origin scenario will require multidimensional, self-consistent modelling, spatially resolved CI observations, and deeper searches for HCO+.

astro-ph.EP↗

arXiv2026

From streamers to stars: overcoming mass loss in protoplanetary disks

Recent high-resolution observations have revealed filamentary accretion flows (``streamers'') in protoplanetary disks older than 1 Myr, suggesting that late-stage interstellar gas infall (late infall) may affect disk evolution and stellar accretion. In Lupus, observations report a positive correlation between ambient gas density and stellar accretion rate. However, it remains unclear whether infall can truly boost stellar accretion, because incoming gas may instead be lost through photoevaporation or magnetically driven disk winds, or remain trapped in the outer disk. We perform one-dimensional long-term ($\sim$1--10 Myr) disk evolution simulations. We first treat late infall as a mass source and then include the effective torque arising from the angular-momentum difference between the infalling gas and Keplerian disk gas. We find that even if substantial gas reaches the outer disk ($\sim 10^{2}$ au), much of it is eventually lost through photoevaporation. Sustained stellar accretion therefore requires efficient inward gas delivery by mechanisms that locally remove angular momentum. Without an effective infall torque, strong viscosity can provide this transport, but it also drives outward angular-momentum transport and excessive disk spreading, inconsistent with the compact disk sizes observed in Lupus. In contrast, MHD disk winds can remove angular momentum without significantly expanding the disk, allowing late infall to sustain stellar accretion while keeping disks compact. Thus, if the Lupus accretion--density correlation is caused by late infall without an effective infall torque, efficient angular-momentum removal by MHD disk winds is required. By contrast, when the effective torque is included, the angular-momentum mismatch itself can promote inward gas transport and enhance stellar accretion, even without strong MHD disk winds.

astro-ph.EP↗

arXiv2021

Gravitational Fragmentation of Extremely Metal-poor Circumstellar Discs

We study the gravitational fragmentation of circumstellar discs accreting extremely metal-poor ($Z \leq 10^{-3}$ Zsun) gas, performing a suite of three-dimensional hydrodynamic simulations using the adaptive mesh refinement code Enzo. We systematically follow the long-term evolution for 2000 years after the first protostar's birth, for the cases of $Z = 0$, $10^{-5}$, $10^{-4}$, and $10^{-3}$ Zsun. We show that evolution of number of self-gravitating clumps qualitatively changes with $Z$. Vigorous fragmentation induced by dust cooling occurs in the metal-poor cases, temporarily providing about 10 self-gravitating clumps at $Z = 10^{-5}$ and $10^{-4}$ Zsun. However, we also show that the fragmentation is a very sporadic process; after an early episode of the fragmentation, the number of clumps continuously decreases as they merge away in these cases. The vigorous fragmentation tends to occur later with the higher $Z$, reflecting that the dust-induced fragmentation is most efficient at the lower density. At $Z = 10^{-3}$ Zsun, as a result, the clump number stays smallest until the disc fragmentation starts in a late stage. We also show that the clump mass distribution also depends on the metallicity. A single or binary clump substantially more massive than the others appear only at $Z = 10^{-3}$ Zsun, whereas they are more evenly distributed in mass at the lower metallicities. We suggest that the disc fragmentation should provide the stellar multiple systems, but their properties drastically change with a tiny amount of metals.

astro-ph.GA↗

arXiv2020

Accretion bursts in low-metallicity protostellar disks

The early evolution of protostellar disks with metallicities in the $Z=1.0-0.01~Z_\odot$ range was studied with a particular emphasis on the strength of gravitational instability and the nature of protostellar accretion in low-metallicity systems. Numerical hydrodynamics simulations in the thin-disk limit were employed that feature separate gas and dust temperatures, and disk mass-loading from the infalling parental cloud cores. Models with cloud cores of similar initial mass and rotation pattern, but distinct metallicity were considered to distinguish the effect of metallicity from that of initial conditions. The early stages of disk evolution in low-metallicity models are characterized by vigorous gravitational instability and fragmentation. Disk instability is sustained by continual mass-loading from the collapsing core. The time period that is covered by this unstable stage is much shorter in the $Z=0.01~Z_\odot$ models as compared to their higher metallicity counterparts thanks to the higher mass infall rates caused by higher gas temperatures (that decouple from lower dust temperatures) in the inner parts of collapsing cores. Protostellar accretion rates are highly variable in the low-metallicity models reflecting a highly dynamical nature of the corresponding protostellar disks. The low-metallicity systems feature short, but energetic episodes of mass accretion caused by infall of inward-migrating gaseous clumps that form via gravitational fragmentation of protostellar disks. These bursts seem to be more numerous and last longer in the $Z=0.1~Z_\odot$ models in comparison to the $Z=0.01~Z_\odot$ case. Variable protostellar accretion with episodic bursts is not a particular feature of solar metallicity disks. It is also inherent to gravitationally unstable disks with metallicities up to 100 times lower than solar.

astro-ph.SR↗

arXiv2015

Formation of primordial supermassive stars by burst accretion

A promising formation channel of SMBHs at redshift 6 is the so-called DC model, which posits that a massive seed BH forms through gravitational collapse of a $\sim 10^5~M_\odot$ SMS. We study the evolution of such a SMS growing by rapid mass accretion. In particular, we examine the impact of time-dependent mass accretion of repeating burst and quiescent phases that are expected to occur with a self-gravitating circumstellar disk. We show that the stellar evolution with such episodic accretion differs qualitatively from that expected with a constant accretion rate, even if the mean accretion rate is the same. Unlike the case of constant mass accretion, whereby the star expands roughly following $R_* \simeq 2.6 \times 10^3 R_\odot (M_*/100~M_\odot)^{1/2}$, the protostar can substantially contract during the quiescent phases between accretion bursts. The stellar effective temperature and ionizing photon emissivity increase accordingly as the star contracts, which can cause strong ionizing feedback and halt the mass accretion onto the star. With a fixed duration of the quiescent phase $Δt_{\rm q}$, such contraction occurs in early evolutionary phases, i.e. for $M_* \lesssim 10^3~M_\odot$ with $Δt_{\rm q} \simeq 10^3$ yr. For later epochs and larger masses but the same $Δt_{\rm q}$, contraction is negligible even during quiescent phases. With larger quiescent times $Δt_{\rm q}$, however, the star continues to contract during quiescent phases even for the higher stellar masses. We show that such behavior is well understood by comparing the interval time and the thermal relaxation time for a bloated surface layer. We conclude that the UV radiative feedback becomes effective if the quiescent phase associated by the burst accretion is longer than $\sim 10^3$ yr, which is possible in an accretion disk forming in the direct collapse model.

astro-ph.SR↗

arXiv2014

Charge density wave soliton liquid

We investigate the charge density wave transport in a quasi-one-dimensional conductor, orthorhombic tantalum trisulfide ($o$-TaS$_3$), by applying a radio-frequency ac voltage. We find a new ac-dc interference spectrum in the differential conductance, which appear on both sides of the zero-bias peak. The frequency and amplitude dependences of the new spectrum do not correspond to those of any usual ac-dc interference spectrum (Shapiro steps). The results suggest that CDW phase dynamics has a hidden degree of freedom. We propose a model in which $2π$ phase solitons behave as liquid. The origin of the new spectrum is that the solitons are depinned from impurity potentials assisted by an ac field when small dc field is applied. Our results provide a new insight as regards our understanding of an elementary process in CDW dynamics.

cond-mat.mes-hall↗

arXiv2006

Hard X-rays from Ultra-Compact HII Regions in W49A

We report the Chandra detection of hard X-ray emission from the Welch ring in W49A, an organized structure of ultra-compact (UC) HII regions containing a dozen nascent early-type stars. Two UC HII regions are associated with hard X-ray emission in a deep Advanced CCD Imaging Spectrometer image exposed for 96.7 ks. One of the two X-ray sources has no near-infrared counterpart and is extended by ~5 arcsec, or ~0.3 pc, at a distance of ~11.4 kpc, which is spatially aligned with the cometary radio continuum emission associated with the UC HII region. The X-ray spectrum of the emission, when fit with a thermal model, indicates a heavily absorbed plasma with extinction of \~5x10^{23}/cm^{2}, temperature of ~7 keV, and X-ray luminosity in the 3.0-8.0 keV band of ~3x10^{33} ergs/s. Both the luminosity and the size of the emission resemble the extended hard emission found in UC HII regions in Sagittarius B2, yet they are smaller by an order of magnitude than the emission found in massive star clusters such as NGC 3603. Three possibilities are discussed for the cause of the hard extended emission in the Welch ring: an ensemble of unresolved point sources, shocked interacting winds of the young O stars, and a wind-blown bubble interacting with ambient cold matter.

astro-ph↗

arXiv2004

Cosmological Growth History of Supermassive Black Holes and Demographics in the High-z Universe : Do Lyman-Break Galaxies Have Supermassive Black Holes?

We study the demographics of supermassive black holes (SMBHs) in the local and high-z universe with hard X-ray luminosity functions (HXLFs) of AGNs. First, we compare the mass accretion history at z>0 with optical luminosity functions (OLFs) and that with HXLFs. We consider the constraints on parameters of mass accretion (energy conversion efficiency and Eddington ratio) and conclude that the constraints based on HXLFs are more adequate rather than that based on OLFs. The sub-Eddington case is allowed only when we use HXLFs. Next, we estimate the upper limit of the cumulative mass density of SMBHs at any redshifts. For an application, we examine if Lyman-Break galaxies (LBGs) at z=3 already have SMBHs in their centers which is suggested by recent observations. If most of LBGs already has massive SMBHs at z=3, the resultant mass density of SMBHs at z=0 should exceed the observational estimate because such SMBHs should further grow by accretion. We show that the special conditions should be met in order that a large part of LBGs have SMBHs (for example, large energy conversion efficiency and frequent mergers and/or direct formations at z>3). The possibility that nearly all LBGs have SMBHs with large mass ratio, such as M_BH/M_stellar > 0.005, is reliably ruled out.(abridged)

astro-ph↗

arXiv2002

Gravitational-Wave Radiation from Magnetized Accretion Disks

The detectability of gravitational wave (GW) radiation from accretion disks is discussed based on various astrophysical contexts. In order to emit GW radiation, the disk shape should lose axial symmetry. We point out that a significant deformation is plausible in non-radiative hot accretion disks because of enhanced magnetic activity, whereas it is unlikely for standard-type cool disks. We have analyzed the 3D magnetohydrodynamical (MHD) simulation data of magnetized accretion flow, finding non-axisymmetric density patterns. The corresponding ellipticity is $ε\sim 0.01$. The expected time variations of GW radiation are overall chaotic, but there is a hint of quasi-periodicity. GW radiation has no interesting consequence, however, in the case of close binaries, because of very tiny disk masses. GW radiation is not significant, either, for AGN because of very slow rotation velocities. The most promising case can be found in gamma-ray bursts or supernovae, in which a massive torus (or disk) with a solar mass or so may be formed around a stellar-mass compact object as the result of a merger of compact objects, or by the fallback of exploded material towards the center in a supernova. Although much more intense GW radiation is expected before the formation of the torus, the detection of GW radiation in the subsequent accretion phase is of great importance, since it will provide a good probe to investigating their central engines.

astro-ph↗

arXiv2002

Constraining the Lifetime of QSOs with Present-day Mass Function of Supermassive Black Holes

Using the theoretical models of the QSO formation, we can reproduce optical QSO luminosity functions (LFs) at high redshifts (z > 2.2). Two different models can reproduce LFs successfully, though the lifetime of QSOs, t_Q, and the relation between the black hole mass and the host halo mass are different each other; t_Q = 10^6yr, in one model, t_Q > 10^7yr, in other models. Here, we propose a method to break this degeneracy. We calculate the mass function of supermassive black holes (SMBHs) at z=2.5, and compare the result with the current mass function obtained by Salucci et al.(1999). In the shorter lifetime model, the mass function at z=2.5 exceeds that of z=0.0 by one order of magnitude, then it should be ruled out. We conclude that the lifetime is at least t_Q > 10^7yr. Next, we examine the difference of the formation epoch of SMBHs existing at z=3.0 for each model under the model assumptions. We simply discuss the difference of formation epoch as another possible model-discriminator.

astro-ph↗

arXiv2002

The relation between the mid-infrared emission and Black Hole Mass in Active Galactic Nuclei: A direct way to probe black hole growth?

We use a large, heterogeneous sample of local active galactic nuclei (AGN) that includes Seyfert 1s, Seyfert 2s and PG quasars to investigate for the first time the relation between black hole mass (M_BH) and mid-infrared nuclear emission. We find a clear relation between M_BH and the 10 micron nuclear luminosity for these local AGNs. There are no significant differences between type 1 and type 2 objects, implying that the reprocessing of the 10 micron nuclear emission is not severely affected by geometric and optical depth effects. We also confirm that M_BH is related to the 2-10keV X-ray luminosity, but only for the Compton thin galaxies. We present a theoretical basis for these empirical relations and discuss possible reasons for the observed scatter. Our results show that rest-frame 10 micron and hard X-ray luminosities (especially the former, which is applicable to all AGN types) can be powerful tools for conducting a census of black hole masses at high redshift and for probing their cosmological evolution.

astro-ph↗

arXiv2001

Theoretical Models of Multi-waveband QSO Luminosity Functions

Cosmological evolution of the QSO luminosity functions (LFs) at NIR/optical/X-ray bands for 1.3 < z < 3.5 is investigated based on the realistic QSO spectra. The accretion-disk theory predicts that although QSO luminosities only depend on mass-accretion rate, \Mdot, QSO spectra have a dependence on black-hole mass, M_{BH}, as well. The smaller M_{BH} is and/or the larger \Mdot is, the harder becomes the QSO NIR/optical/UV spectrum. We model disk spectra which can reproduce these features and calculated LFs for redshift z ~ 3 with the assumption of new-born QSOs being shining at the Eddington luminosity. The main results are: (i) the observed LFs at optical and X-rays can be simultaneously reproduced. (ii) LFs at optical and X-ray bands are not sensitive to M_{BH}, while LFs at NIR bands are; about one order of magnitude difference is expected in volume number densities at L_{I, J} ~ 10^{46} erg s^{-1} between the case that all QSOs would have the same spectral shape as that of M_{BH} = 10^{9} M_sun and the case with M_{BH} = 10^{11} M_sun. (iii) The resultant LFs at NIR are dominated by 10^{7} M_sun black-holes at L_{I, J} ~ 10^{44} erg s^{-1}, and by 10^{11} M_sun black-holes at L_{I, J} \~ 10^{46} erg s^{-1}. Future infrared observations from space(e.g.NGST) will probe cosmological evolution of black hole masses. For redshift z < 3, on the other hand, the observed optical/X-ray LFs can be fitted, if the initial QSO luminosity L_0 is below the Eddington luminosity. Interestingly, the best fitting values of l = L_0/L_{Edd} are different in B- and X-ray bands; l_B ~ 2.5 l_X. The reason for this discrepancy is briefly discussed.

astro-ph↗

arXiv2000

Anisotropic charge transfer mechanism in La$_{2-x}$Sr$_x$CuO$_4$ and Bi$_2$Sr$_2$Ca$_{1-x}$Y$_x$Cu$_2$O$_{8+δ}$

Raman spectra of La$_{2-x}$Sr$_x$CuO$_4$ are similar to those of Bi$_2$Sr$_2$CaCu$_2$O$_{8+δ}$ except for the split two-magnon peaks at the stripe phase and the stronger step-like decrease in the low energy $B_{\rm 2g}$ spectra. The suppressed $B_{\rm 1g}$ spectral region below the two-magnon peak decreases as the carrier density increases, whereas the energy of the step-like suppression is little dependent on the carrier density. It suggests the anisotropic charge transfer mechanism coupled with magnetic excitations along the nearest neighbor Cu sites and the phononic excitations along the diagonal direction.

cond-mat.supr-con↗

arXiv1999

Relation between the superconducting gap energy and the two-magnon Raman peak energy in Bi2Sr2Ca{1-x}YxCu2O{8+δ}

The relation between the electronic excitation and the magnetic excitation for the superconductivity in Bi2Sr2Ca{1-x}YxCu2O{8+δ} was investigated by wide-energy Raman spectroscopy. In the underdoping region the B1g scattering intensity is depleted below the two-magnon peak energy due to the "hot spots" effects. The depleted region decreases according to the decrease of the two-magnon peak energy, as the carrier concentration ncreases. This two-magnon peak energy also determines the B1g superconducting gap energy as $2Δ\approx α\hbar ω_{\rm Two-Magnon} \approx J_{\rm effective}$ $(α=0.34-0.41)$ from under to overdoping hole concentration.

cond-mat.supr-con↗