__ASTRONOMY__magazine article entitled '

*Speaking the Language of the Universe*' (December, p. 24) is one every math phobe needs to read- especially people who also appreciate the wonders of the night sky.

But sadly, as the piece by Bob Berman observes, while "

*professional astronomers use math all the time*" - see e.g. some of the (free) journal articles here:

http://iopscience.iop.org/0004-637X/743/2

Hobby astronomers generally "

*don't have math in their bones*". As Berman adds:

*"They hate the subject. Perhaps it reminds them of school. Square roots and standard deviations bog down articles for them, and science writers oblige by leaving out equations altogether*."

Which is sad beyond measure, because indeed, as Berman goes on to show, math is the language of the universe. Sure it's easy to simply stand beneath the stars and simply gaze at galaxies, planets and the Moon through a telescope - Oooh-ing and ahh-ing all the time. But while wonder and awe can be the keynote at that level, it can't lead to any deeper understanding of what those objects actually are, what they're made of, how they move or how they might affect our planet. For that, deeper analysis is needed, i.e. into the relationships between physical parameters that define them.

Just to know how distant an object is - say a nearby star- depends on math, and it is critical given that the distance can allow other properties to be determined. Consider the famous "

__parallax method__" to obtain the distance to nearby stars. This method can apply to all stars within a distance of maybe 50 parsecs (1 pc = 3.26 Ly) or those for which a measurable parallax angle p exists. The geometry shown below is useful to this end:

D = r/ tan (p)

The relationship is such that for p = 1 arcsec the distance of the star would be 1 parsec (e.g.

**par**-allax

**sec**-ond). an angle of 1 arcsec = 1" = 1/3600 degree. So we see it is an extremely tiny angle. similarly, if the angle p = 1/10" then D = 10 parsecs, so we perceive a reciprocal relationship such that D = 1/p", though we must ensure the units are consistent.

In many applications, such as the budding undergrad student meets in 1st year Astronomy, the parallax angle p is merged with the equation for the

*"distance modulus*" - which makes use of the absolute magnitude M (see previous blog on this) and apparent magnitude m. In this way, estimates of the star's energy output, and brightness can be made.

Then, if D is the distance, the usual expression for distance modulus is:

(m - M) = 5 log (D/10) = 5 log D - 5 log 10 = 5 log D - 5

But: D = 1/p

so:

(m - M) = 5 log (1/p) - 5

Or: (m - M) + 5 = 5 log p

A sample problem, such as an Astronomy 201-202 student would have to do for homework, is as follows:

Barnard's star has an absolute magnitude of +13.2 and an apparent magnitude m = +9.5. Find its distance in LIGHT YEARS.

The solution is based on using the parsec form of the distance modulus:

Then:

(m - M) = 5 log (1/p) - 5

(9.5 - 13.2) = 5 log(1/p) - 5

-3.7 = 5 log (1/p) - 5

5 log (1/p) = (5 - 3.7) = 1.3

log (1/p) = (1.3)/5 = 0.26

Taking anti-logs:

1/p = D = 1.81 pc

But 1 pc = 3.26 Ly, so D = (1.81 pc)(3.26 Ly/pc) = 5. 9 LY

**Spherical Astronomy:**

It is based on the projection of the Earth's N. and S. poles into the sky, as well as its equator. The poles then become the

*North and South Celestial poles*, and the equator becomes the

*celestial equator*. If these poles are defined respectively at +90 degrees (NCP) and -90 degrees (SCP) and the celestial equator at 0 degrees, then a consistent system of celestial latitude and longitude can be defined in a consistent system, to locate any celestial object. We call the longitude coordinate (Θ) the Right Ascension (R.A.) while the celestial latitude coordinate is called declination and is measured in degrees north or south of the celestial equator. (In the diagram, the complementary angle of the declination is shown, φ, which we call the

*zenith distance*.)

*hour angle*- and distinguish it from the Right Ascension. This starts with identifying the R.A. of his local meridian (the imaginary celestial longitude passing through his zenith or highest point.) The Right Ascension of the star is clearly equal to the local sidereal time (L.S.T.) plus the hour angle. Thus, we can write: HA = RA of observer meridian - RA of object

Of course, before he gets very far, he will be adept at sketching any number of diagrams to solve time and position problems, such as the diagram below - with perspective looking down onto the North Celestial pole:

The budding astronomy student will also have to know how to sketch a three dimensional diagram to enable conversion between coordinates, say from the horizontal (observer -based) to the celestial sphere. This will always include what is called the fundamental "

**astronomical triangle**" (shaded region of Fig. 3 below):

We have for the law of sines:

Sin A/ sin a = sin B/ sin b = sin C/ sin c

where A, B, C denote ANGLES and a,b,c denote measured arcs. (Note: we could also have written these by flipping the numerators and denominators).

We have for the law of cosines:

cos a = cos b cos c + sin b sin c cos A

Where a, b, c have the same meanings, and of course, we could write the same relationship out for any included angle.

Now, we use Fig. 3, for a celestial sphere application, in which we use the spherical trig relations to obtain an astronomical measurement.

Using the angles shown in Fig. 3 each of the angles for the law of cosines (given above) can be found. They are as follows:

cos a = cos (90 deg - decl.)

where decl. = declination

cos b = cos (90 deg - Lat)

where 'Lat' denotes the latitude. (Recall from Fig. 1 if φ is polar distance (which can also be zenith distance) then φ = (90 - Lat))

cos c = cos z

where z here is the zenith distance.

sin b = sin (90 deg - Lat)

sin c = sin z

and finally,

cos A = cos A

where A is

*azimuth.*

Let's say we want to find the declination of the star if the observer's latitude is 45 degrees N, and the azimuth of the star is measured to be 60 degrees, with its zenith distance z = 30 degrees. Then one would solve for cos a:

cos a = cos (90 deg - decl.)=

cos (90 deg - Lat) cos z + sin (90 deg - Lat) sin z cos (A)

cos (90 deg - decl.) =

cos (90 deg - decl.)= cos (45) cos 30 + sin (45) sin 30 cos 60

We know, or can use tables or calculator to find:

cos 45 = Ö2/ 2

cos 30 = Ö3 / 2

sin 45 = Ö2 / 2

sin 30 = ½

cos 60 = ½

Then:

cos (90 deg - decl.)= [Ö6/ 4 + Ö2/ 8]

cos (90 deg - decl.)= 0.789

arc cos (90 deg - decl.)= 37.9 deg

Then:

decl. = 90 deg - 37.9 deg = 52.1 deg

Or, decl. (star) = + 52.1 degrees

(x)

(y)

(z) u,v =

(cos v .....cos u)

(cos v .....sin u)

(sin v..............)

After conversion the curvilinear coordinates may be calculated according to:

u = arctan (y/x) and v = arcsin (z)

Now, consider conventional orthogonal matrices of 3 x 3 dimensions, given as functions: R1(Θ), R2(Θ) and R3(Θ), to rotate the general system by the angle Θ about axes x, y and z, respectively. Thus we obtain:

R1(Θ) =

(1..........0................0)

(0.....cos(Θ)..... sin(Θ))

(0......-sin(Θ)....cos(Θ))

R2(Θ) =

(cos (Θ)......0........- sin(Θ))

(0................1...............0.. )

(sin(Θ)........0.......cos(Θ) )

R3(Θ) =

(cos(Θ)..........sin(Θ)..........0)

(-sin (Θ)......cos(Θ)...........0)

(0 ..................0..................1)

To fix ideas, say you wish to obtain the horizontal coordinates (A, a) for some object in the sky and you know its R.A. and decl. from an almanac. Then the procedure is fairly straightforward, and entails writing:

R2(Θ) = R2(90 - lat.)

so that:

(x)

(y)

(z) A,a =

**R3(-180 deg) R2(90 - lat.) (XYZ(h, decl.))**

(x)

(y)

(z) h,decl.

(cos 180........-sin 180................0)

(sin 180........cos 180................0)

(0......................0......................1)

And:R3(Θ) =

(cos(Θ)..........sin(Θ)..........0)

(-sin (Θ)......cos(Θ)...........0)

(0 ..................0..................1)

Therefore: R3(-180) =

(-1.....0.......0)

(0.......-1.....0)

(0.......0.......1)

Obtaining R2(Θ) = R2(90 - lat.) is just as easy, if one recalls the basic trig identity:

cos (90 - φ) = sin (φ)

**Astrophysics:**

In Introductory Astrophysics, the primary emphasis is getting the student acquainted with the Planck function and applying it to simple, plane-parallel stellar atmospheres, such as depicted below:

^{2})/ l

^{5}} [1/ exp (hc/lkT) - 1)]

dI(l)/ds = -k(l) I(l) + k(l) S(l)

= k(l) [S(l) – I(l)] - 0 or I(l) = S(l)

For

**, the student learns I(l) equals the Planck function:**

*a black body*B(l) : i.e. S(l) = I(l) = B(l)

And this is a condition which implies LOCAL THERMODYNAMIC EQUILIBRIUM or

*LTE does NOT mean complete thermodynamic equilibrium!(E.g. since in the outer layers of a star there is always large energy loss from the stellar surface) . Thus, one only assumes the emission of the radiation is the same as for a gas in thermodynamic equilibrium at a temperature (T) corresponding to the temperature of the layer under consideration. Another way to say this is that if LTE holds, the photons always emerge at all wavelengths. In the above treatment, note that the absorption coefficient was always written as: k(l) to emphasize its wavelength (l) dependence.*

**LTE**The student will be required to do a number of challenging problems for homework, including the specific applications of the gray atmosphere approximation. In a particular integral, let the surface flux:

_{o}) = 2 p (I(cos (q)) = p [a(l) + 2(b(l)/3 ]

and F

_{lo}= S(l) t(l) = 2/3

which states that the flux coming

*out of the stellar surface*is equal to the source function at the

*optical depth*t

*= 2/3*. This is the very important ‘

*Eddington-Barbier’ relation*that facilitates an understanding of how stellar spectra are formed. Once one then assumes LTE, one can further assume k(l) is independent of l (gray atmosphere) so that:

k(l) = k; t (l) = t and F

_{lo}= B

_{l}(T(t = 2/3) )

Thus, the energy distribution of F

_{l}is that of a black body corresponding to the temperature at an optical depth t = 2/3. From this, along with some simple substitutions and integrations a wdie array of problems can be done. A few HW problem examples:

1. Estimate the specific intensity I (q=p/4) if the surface flux from the Sun is 6.3 x 10

^{7}Jm

^{-2}s

^{-1}.

2. Find the effective temperature of the Sun and the boundary temperature (T

_{o}) and account for any difference. (Hint: The effective temperature is related to the boundary temperature by: T

_{eff }

^{ }= (2)

^{1/4}T

_{o}

_{ })

*specific intensity*i.e.

I

_{l}

_{ }(0,q) = ò

_{o}

^{z }B

_{l}(t) exp [(-t

_{l}

_{ }/ cos q)] dt/ cos q

where B

_{l}(t) is the Planck function. The energy which flows per unit solid angle will then be based upon finding:

dE n = I cos q dw dt dn

from which one will wish to obtain the

*total flux*.

By now radio astronomy will emerge, with essentials of assorted radio telescope properties, especially for antennas, will also be introduced, along with many problems - including practical (i.e. designing a specific antenna to detect an object of given flux, and spectral output etc.). To this end the student will distinguish between the flux emitted for an isotropic (lossless) antenna, and an anisotropic antenna with the gain (g) subject to the constraint:

_{4}

_{p}g dw = 4p

and the relation between the gain of the antenna and its effective aperture (A) such that:

g( (q , φ ) = 4p A (q , φ)/ l

^{2}

From here, the student will be expected to work out the beam width and beam efficiency of a given antenna, as well as compute the 'brightness temperature' for a localized source, and the antenna temperature:

_{4}

_{p}g T(b) dw

Sensitivity of the antenna will also be considered, as well as other details such as the amplification of high frequency signals.

F = G M(r) r dr/ r

^{2}

Since the attraction due to the material outside r is zero, we should have for equilibrium: - dP = G M(r) r dr/ r

^{2}

Or: dP/dr = - G M(r) r / r

^{2}

Consider now the mass of the shell between an outer layer of a given star and a deeper stellar layer. This is approximately, 4p r

^{2 }r dr, provided that dr (shell thickness) is small. The mass of the layer is the difference between M(r + dr) and M(r) which for a thin shell is:

^{2 }r

The two equations, for dP/dr and dM/dr represent the basic equations of stellar structure, without which the innards of a star would be inaccessible to investigation. A third equation of stellar structure may be derived using by using the equation for dM/dr in combination with the fact that a star’s luminosity is produced through the consumption of its own mass. This may be expressed mathematically as:

where e denotes the

*rate of energy generation*. For the proton-proton cycle (for stars like the Sun- and

*designed for cgs units*!):

^{6}(r X

^{2}).· (10

^{6}/T)

^{2/3}exp[-33.8(10

^{6}/T)

^{1/3}]

Of course, to construct a stellar model as part of a course project, the student will more likely have to deal with a different 'critter' entirely - say a star of two solar masses with a

*convective*(as opposed to a radiative) core and with composition: X = 0.65 (i.e. 65% hydrogen), Y = 0.32 (i.e. 32% helium) and Z = 0.03 (i.e. 3 % heavy elements). Say with an energy generation function:

e= 10

^{-14.2}(r X X(CN)).· (T

^{20})

where: X(CN) = 0.01 and :

X = 4.34 x 10

^{25}Z(1 + X) r T

^{--3.5}

This is none other than the stellar model problem construction I had to complete, and for which I received an 'A' and also an A in the course. The details of the problem were:

Neglect radiation pressure and degeneracy and assume the gas is nearly totally ionized. Utilizing Wrubel's interior integrations and Schwarzschild's and Harm's envelop solutions:

a) Construct a consistent stellar model utilizing the U-V plane fitting technique, and

b) Calculate the following physical properties of the star: L, R, T

_{c}, r

_{c}, P

_{c}, and the mass of the convective core, m

_{c}.

Still want to become an Astronomy major? Just make sure math is in your blood.

*Math Drives The Universe*', in November, 2013)