662 research outputs found
A process-based analysis of ocean heat uptake in an AOGCM with an eddy-permitting ocean component
About 90% of the anthropogenic increase in heat stored in the climate system is found the oceans. Therefore it is relevant to understand the details of ocean heat uptake. Here we present a detailed, process-based analysis of ocean heat uptake (OHU) processes in HiGEM1.2, an atmosphere-ocean general circulation model (AOGCM) with an eddy-permitting ocean component of 1/3 degree resolution. Similarly to various other models, HiGEM1.2 shows that the global heat budget is dominated by a downward advection of heat compensated by upward isopycnal diffusion. Only in
the upper tropical ocean do we find the classical balance between downward diapycnal diffusion and upward advection of heat. The upward isopycnal diffusion of heat is located mostly in the Southern Ocean, which thus dominates the global heat budget.
We compare the responses to a 4xCO2 forcing and an enhancement of the windstress forcing in the Southern Ocean. This highlights the importance of regional processes for the global ocean heat uptake. These are mainly surface fluxes and convection in the high latitudes, and advection in the Southern Ocean mid-latitudes. Changes in diffusion are less important.
In line with the CMIP5 models, HiGEM1.2 shows a band of strong OHU in the mid-latitude Southern Ocean in the 4xCO2 run, which is mostly advective. By contrast, in the high-latitude Southern Ocean regions it is the suppression of convection that leads to OHU. In the enhanced windstress run, convection is strengthened at high Southern latitudes, leading to heat loss, while the magnitude of the OHU in the Southern mid-latitudes is very similar to the 4xCO2 results. Remarkably, there is only very small global OHU in the enhanced windstress run. The wind stress forcing just leads to a redistribution of heat.
We relate the ocean changes at high southern latitudes to the effect of climate change on the Antarctic Circumpolar Current (ACC). It weakens in the 4xCO2 run and strengthens in the wind stress run. The weakening is due to a narrowing of the ACC, caused by an expansion of the Weddell Gyre, and a flattening of the isopycnals, which are explained by a combination of the wind stress forcing and increased precipitation
Ocean heat uptake and its consequences for the magnitude of sea level rise and climate change
Under increasing greenhouse gas concentrations, ocean heat uptake moderates
the rate of climate change, and thermal expansion makes a substantial contribution to sea level rise. In this paper we quantify the differences in projections
among atmosphere-ocean general circulation models of the Coupled Model Intercomparison Project in terms of transient climate response, ocean heat uptake
efficiency and expansion efficiency of heat. The CMIP3 and CMIP5 ensembles
have statistically indistinguishable distributions in these parameters. The ocean
heat uptake efficiency varies by a factor of two across the models, explaining
about 50% of the spread in ocean heat uptake in CMIP5 models with CO2 increasing at 1%/year. It correlates with the ocean global-mean vertical profiles
both of temperature and of temperature change, and comparison with observations suggests the models may overestimate ocean heat uptake and underestimate surface warming, because their stratification is too weak. The models
agree on the location of maxima of shallow ocean heat uptake (above 700 m) in
the Southern Ocean and the North Atlantic, and on deep ocean heat uptake (below 2000 m) in areas of the Southern Ocean, in some places amounting to 40%
of the top-to-bottom integral in the CMIP3 SRES A1B scenario. The Southern Ocean dominates global ocean heat uptake; consequently the eddy-induced
thickness diffusivity parameter, which is particularly influential in the Southern
Ocean, correlates with the ocean heat uptake efficiency. The thermal expansion
produced by ocean heat uptake is 0.12 m YJ−1, with an uncertainty of about
10% (1 YJ = 1024 J)
Host galaxies of bright high redshift quasars: Luminosities and colours
We present the results of a near-infrared imaging study of high redshift
(z~3) quasars using the ESO-VLT. Our targets were selected to have luminosities
among the highest known (absolute magnitude M_B <~ -28. We searched for
resolved structures underlying the bright point-source nuclei by comparing the
QSO images with stars located in the same fields. Two QSOs (HE2348-1444 at
z=2.904 and HE2355-5457 at z=2.933) are clearly resolved in K_S, and with
somewhat lower significance also in H; one object is resolved only in K_S. At
these redshifts, H and K_S correspond almost exactlly to rest-frame B and V,
respectively, with virtually no K-correction. We also report briefly the
non-detection of some additional QSOs. The detected host galaxies are extremely
luminous with M_V ~ -25. Their rest-frame B-V colours, however, are close to
zero in the Vega system, indicating substantial contributions from young stars
and a stellar mass-to-light ratio below 1 (in solar units). Tentatively
converting M_V and B-V into rough estimates of stellar masses, we obtain values
of M_star in the range of several 10^11 M_sun, placing them within the
high-mass range of recent high-redshift galaxy surveys. We present optical
spectra and use CIV line width measurements to predict virial black hole
masses, obtaining typical values of M_bh ~ 5x10^9 M_sun. With respect to the
known correlation between host galaxy luminosity L_V(host) and M_bh, our
measurements reach to higher luminosities and redshifts than previous studies,
but are completely consistent with them. Comparing our objects with the local
(z~0) M_bh - M_bulge relation and taking also the low stellar mass-to-light
ratios into account, we find tentative evidence for an excess in the
M_bh/M_bulge mass ratio at z~3.Comment: 9 pages, 7 figures, accepted for publication in A&
Resistivity in warm dense plasmas beyond the average-atom model
The exploration of atomic properties of strongly coupled partially degenerate
plasmas, also referred to as warm dense matter, is important in astrophysics,
since this thermodynamic regime is encountered for instance in Jovian planets'
interior. One of the most important issues is the need for accurate equations
of state and transport coefficients. The Ziman formula has been widely used for
the computation of the static (DC) electrical resistivity. Usually, the
calculations are based on the continuum wavefunctions computed in the
temperature and density-dependent self-consistent potential of a fictive atom,
representing the average ionization state of the plasma (average-atom model).
We present calculations of the electrical resistivity of a plasma based on the
superconfiguration (SC) formalism. In this modeling, the contributions of all
the electronic configurations are taken into account. It is possible to obtain
all the situations between the two limiting cases: detailed configurations (a
super-orbital is a single orbital) and detailed ions (all orbitals are gathered
in the same super-orbital). The ingredients necessary for the calculation are
computed in a self-consistent manner for each SC, using a density-functional
description of the electrons. Electron exchange-correlation is handled in the
local-density approximation. The momentum transfer cross-sections are
calculated by using the phase shifts of the continuum electron wavefunctions
computed, in the potential of each SC, by the Schroedinger equation with
relativistic corrections (Pauli approximation). Comparisons with experimental
data are also presented.Comment: submitted to "Contributions to Plasma Physics
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