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From Gray et al. (2010)

From Gray et al. (2010)

Solar irradiance (or the flux of the Sun’s output directed toward Earth) provides virtually 100% of the energy received and absorbed by the Earth system. So it shouldn’t be any surprise that if you open up an elementary climate change textbook and search for suitable candidates that can actually cause the global climate to vary in time, changes in sunlight will be on the list (along with volcanic eruptions, land use changes, anthropogenic greenhouse gas emissions, etc).

When one actually targets specific past climate change “events,” however, changes in sunlight rarely enter the picture in any appreciable way. It is not self-evident that this should be the case, but we seem to be rather fortunate in orbiting a well-behaved star that only exhibits changes in output on the order of a tenth of a percent or so on decadal-to-centennial timescales. See the record below, for instance. Various choices for solar forcing used by groups in the recent (CMIP5/PMIP3) generation of climate simulations for the last millennium can be found in Figure 8 of Schmidt et al., 2011. Note the vertical scales. We’ll come back to some of the features in the plot below.


From http://lasp.colorado.edu/home/sorce/data/tsi-data/

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Temperature trend 1960–2012 versus latitude and pressure. The value for each latitude and pressure is the medians of the trends at individual stations in that (10°) latitude bin. Units are °C per decade. From Sherwood and Nishant (2015).

Temperature trend 1960–2012 versus latitude and pressure. The value for each latitude and pressure is the medians of the trends at individual stations in that (10°) latitude bin. Units are °C per decade. From Sherwood and Nishant (2015).

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In this post, I’ll revisit the simple two-layer column model described in the last post. This time we’ll use the model as a way to start thinking about the way we define “climate feedback.”

The top-of-the-atmosphere energy budget has been the vehicle we’ve employed in order to explore how planets come into equilibrium with radiation from their stellar host, and here we wish to further investigate how that equilibrium is obtained. It follows that we ought to be interested in how the outgoing longwave radiation (OLR) varies with surface temperature. By now, you are hopefully familiar with the fact that increasing emissivity (i.e., the greenhouse effect) in the atmospheric column will reduce OLR by shifting the mean emission height to higher, colder levels (keeping temperatures held fixed). We call this radiative forcing, or the instantaneous effect of the increase in column absorption on emission to space. Furthermore, we also know that the temperatures must then increase in order for the OLR to return to its original value. We’ll assume that shortwave absorption by the planet is unchanged, so the OLR (at equilibrium) in the “perturbed emissivity” climate is exactly identical to the value in the unperturbed climate. That zero anomaly in OLR can thus be decomposed into two parts- the radiative forcing that decreased OLR, and an equal but opposite flux that arises from all changes that occurred in the column to get back to equilibrium. It is the latter we’d like to further diagnose, and hopefully make contact with how scientists actually use models operationally in order to quantify feedbacks.

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I have been absent from writing this blog for nearly two years, which sometimes happens when one has an interest in starting a blog. This is a post I felt was worth writing down though. Some of the context might not be entirely clear to those who haven’t gone through an atmospheric science program or picked up some textbooks dealing with climate physics, so I will try to clear that up.

I will try to outline what I feel can be improved in practical instruction of the greenhouse effect, just based on some modification to a toy model that has already been employed in many classrooms and textbooks (some examples are Atmosphere, Ocean and, Climate Dynamics; Global Physical Climatology; Global Warming: Understanding the forecast, all great reads by the way). The framing here can be presented to an upper-undergraduate or graduate classroom, but the calculus can be stripped away for courses with minimal math requirements. Here, my focus is in making better contact with how the greenhouse effect actually works rather than going through algebraic exercises that yield numbers which don’t have any particular special meaning.
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In discussions of climate change, it is often useful to think about the transition of the climate from one state to another, and ask how the magnitude of the response is related to changes in a control parameter (such as the solar constant, or CO2 concentration). This is the classical problem of climate sensitivity, which is intimately connected with assessing the degree to which Earth has the capacity to change. In such an analysis, we typically begin by reducing the “climate” to a single variable, commonly global mean temperature (T), and gauge its evolution as a function of the control parameter. Of general interest to society, for example, is how the global mean temperature responds to changes in CO2 concentration. I will build up some theoretical background into climate sensitivity in this article, and move on to observations and modeling results in subsequent posts.

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Introduction

Welcome to ClimatePhys. Please see the Introduction and Blog Rules for an expanded version of the site’s purpose and intended readership. The goal of this site is to provide a technical forum for discussions of planetary climate, climate change, and the governing dynamics that ultimately dictates the behavior of atmospheres. Some attention will be given to the issue of modern-day climate change, although my mission is to focus on a broader class of issues that can be generalized to any time period or even some hypothetical planet. There are, however, a number of key events in Earth’s past that are worth mentioning specifically and I will do so when appropriate.

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