Image 1 Caption: A cartoon explicating the Stefan-Boltzmann law in brief. For a more detailed explication, see below.
Features:
The logarithmic Stefan-Boltzmann law is
Table: Blackbody Radiators.
Blackbody Radiator T F Comment (K) (W/m**2)
CMB-like 2.7260 3.131*10**(-6) The CMB has a blackbody spectrum, but there is no radiating surface in the modern observable universe. Human-body-like 310 5.237*10**2 But the human body does NOT radiate this much (see the note below). Sun-like 5772 6.294*10**7 The Sun does almost radiate like this at the effective temperature T = 5772 K.
The effective temperature T_eff
of a star
is the temperature
of a blackbody radiator
that radiated exactly the
luminosity L
of the star
from a spherical surface of exactly a well-defined characteristic
radius
for the star's
photosphere:
i.e., the
photospheric radius R_ph.
The formulae for
effective temperature are:
In general, the
effective temperature is harder
to determine than
color temperature.
A human body
approximated as a cylinder
has surface area
∼ h*2πr ≅ 1.5*6*0.2 ≅ 2 m**2.
Thus, according to the above table if it radiated like
a blackbody radiator,
it should radiate ∼ 1000 W.
But the human body
is surrounded by an ambient medium at typically ∼ 300 K
and the radiation field and
heat conduction
from the ambient medium is sufficient to transfer heat to
the human body
to maintain a temperature ∼ 300 K.
Upshot is that the
human body
radiates a DILUTED
blackbody radiation field:
it has approximately a
blackbody spectrum shape
for temperature ∼310 K, but
has much less radiant flux
than a blackbody radiation field
of ∼310 K.
So the human body does NOT lose
heat energy at rate of
∼ 1000 W.
But how much radiant flux
does the human body
radiate?
The basal metabolic rate (BMR)
for humans is the minimal
rate of energy generation in
and therefore the minimal heat energy loss from
the human body.
The energy generation comes from
food energy
(i.e., the chemical energy of
food).
The
basal metabolic rate average ≅ 73 W
is obviously much less than the flux
from the
human-body-like
blackbody radiator in the above
Table: Blackbody Radiators.
For some information from 2019 on
the human body
metabolic rate,
see BBC: Ultimate limit of human endurance found,
2019,
Thurber et al. (2019),
and references therein.
L = (4πR_ph)*F = (4πR_ph)*σT_eff**4 and T_eff = [L/(4πR_ph*σ)]**(1/4) ,
where we have used the
Stefan-Boltzmann law F=σ*T**4
for blackbody radiation.
However, there are complications in evaluating
effective temperature:
There are various ways of dealing with these complications which are beyond our scope.
     
What is called the
color temperature
of a star is based on fitting
a blackbody spectrum to
the star's
spectrum.
There are various ways of the doing the fit which give somewhat different answers.
The fit can be done using
Wien's law
or color indices.
     
Since a star is NOT exactly
a blackbody radiator
with a radius equal to the
aforesaid well-defined characteristic
photospheric radius, the
color temperature
will NOT in general equal the
effective temperature.
In fact, the
color temperature
is usually a bit higher.
     
The effective temperature
is preferred over
color temperature
for the definition of the standard
photospheric temperature
because the
effective temperature
has a perfectly meaning for
a photosphere in special ideal case
that many stars actually approach:
i.e., the case of a grey atmosphere
in
local
thermodynamic equilibrium (LTE)
(Wikipedia:
Grey atmosphere: Temperature solution;
Mi-55,72).
     
The temperature
for the Sun given in
Table: Blackbody Radiators
5772 K
is the effective temperature.
For the Sun, the
color temperature
(from some determination method) is ∼ 5900 K
(Wikipedia: Color temperature: Sun)
which is, indeed, a bit higher than the
Sun
effective temperature 5772 K.