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R. A. Wood

Publications and source records attributed to R. A. Wood.

2 recordsLinked to original sources

Quantifying risk of a noise-induced AMOC collapse from northern and tropical Atlantic Ocean variability

The Atlantic Meridional Overturning Circulation (AMOC) exerts a major influence on global climate. There is much debate about whether the current strong AMOC may collapse as a result of anthropogenic forcing and/or internal variability. Increasing the noise in simple salt-advection models can change the apparent AMOC tipping threshold. However, it's not clear if 'present-day' variability is strong enough to induce a collapse. Here, we investigate how internal variability affects the likelihood of AMOC collapse. We examine internal variability of basin-scale salinities and temperatures in four CMIP6 pre-industrial simulations. We fit this to an empirical, process-based AMOC box model, and find that noise-induced AMOC collapse (defined as a decade in which the mean AMOC strength falls below 5 Sv) is unlikely for pre-industrial CMIP6 variability unless external forcing shifts the AMOC closer to a threshold. However, CMIP6 models seem to underestimate present-day Atlantic Ocean variability, and stronger variability substantially increases the likelihood of noise-induced collapse, especially if forcing brings the AMOC close to a stability threshold. Surprisingly, we find a case where forcing temporarily overshoots a stability threshold but noise decreases the probability of collapse. Accurately modelling internal decadal variability is essential for understanding the increased uncertainty in AMOC projections.

physics.ao-ph↗

The Infall of the Virgo Elliptical Galaxy M60 toward M87 and the Gaseous Structures Produced by Kelvin-Helmholtz Instabilities

We present Chandra observations of hot gas structures, characteristic of gas stripping during infall, in the Virgo cluster elliptical galaxy M60 (NGC4649) located $1$ Mpc east of M87. $0.5-2$ keV Chandra X-ray images show a sharp leading edge in the surface brightness $12.4 \pm 0.1$ kpc north and west of the galaxy center in the direction of M87 characteristic of a merger cold front due to M60's motion through the Virgo ICM. We measured a temperature of $1.00 \pm 0.02$ keV for abundance $0.5 Z_\odot$ inside the edge and $1.37^{+0.35}_{-0.19}$ keV for abundance $0.1 Z_\odot$ in the Virgo ICM free stream region. We find that the observed jump in surface brightness yields a density ratio of $6.44^{+1.04}_{-0.67}$ between gas inside the edge and in the cluster free stream region. If the edge is a cold front due solely to the infall of M60 in the direction of M87, we find a pressure ratio of $4.7^{+1.7}_{-1.4}$ and Mach number $1.7 \pm 0.3$. For 1.37 keV Virgo gas we find a total infall velocity for M60 of $1030 \pm 180$ kms$^{-1}$. We calculate the motion in the plane of the sky to be $1012^{+183}_{-192}$ km$^{-1}$ implying an inclination angle $ΞΎ= 11 \pm 3$ degrees. Surface brightness profiles show the presence of a faint diffuse gaseous tail. We identify filamentary, gaseous wing structures caused by the galaxy's motion through the ICM. The structure and dimensions of these wings are consistent with simulations of Kelvin-Helmholtz instabilities as expected if the gas stripping is close to inviscid.

astro-ph.GA↗