Showing posts with label relativity. Show all posts
Showing posts with label relativity. Show all posts

Sunday, March 10, 2024

Fun with the TI-81 (March 2024 Edition)

Fun with the TI-81 (March 2024 Edition)






TI-81 SCATTER







Produces a scatter plot.


Size: 52 bytes


Code:


If Dim{x}=0

Disp “NO DATA”

If Dim{x}=0

Stop

ClrDraw

1→I

Lbl 0

PT-On({x}(I),{y}(I))

IS>(I,Dim{x})

Goto 0

DispGraph


Note: Dim{x} returns the number of data points in the statistics list {x}.

Keystrokes: [ VARS ], DIM, 7: Dim{x}



TI-81 ANGLES


Given three pints, the internal and external angle are calculated.





Size: 196 bytes


Code:

Deg

Disp “SIDE PT (S,T)”

Input S

Input T

Disp “CORNER (M,N)”

Input M

Input N

Disp “SIDE PT (U,V)”

Input U

Input V

(S-M)*(U-M)+(T-N)*(V-N)→D

√((S-M)^2+(T-N)^2)→A

√((U-M)^2+(V-M)^2)→B

cos^-1 (D/(A*B))→I

360-I→E

Disp “INTERNAL ANGLE”

Disp I

Disp “EXTERNAL ANGLE”

Disp E



Example:

(S,T) = (-4,-6)

(M,N) = (1,1)

(U,V) = (3,5)



INTERNAL ANGLE: 171.0273734

EXTERNAL ANGLE: 188.9726266


Source:

Cook, John D. “Ramanujan approximation for circumference of ellipse” John D. Cook Consulting. May 5, 2015. https://www.johndcook.com/blog/2013/05/05/ramanujan-circumference-ellipse/ Accessed January 24, 2024


TI-81 ELLIPSE

Given the length of the semi-axis, the program draws the ellipse, calculates the area, and approximates the circumference using Ramanujan formula.

Size: 195 bytes


Code:


Param

Rad

Disp “SEMI X-AXIS”

Input A

Disp “SEMI Y-AXIS”

Input B

(A-B)/(A+B)→L

π*(A+B)*(1+(3*L^2)/(10+√(4-3*L^2))→P

π*A*B→R

Disp “APPROX. CIR=”

Disp P

Disp “AREA=”

Disp R

Pause

All-Off

“A*cos T”→X_1T

“B*sin T”→Y_1T

X1T-On

-A-1→Xmin

A+1→Xmax

-B-1→Ymin

B+1→Ymax

0→Tmin

2π→Tmax

π/24→Tstep

DispGraph



Notes:

All-Off turns all the graphing equations off from graphing.

[ 2nd ] {Y-VARS}, OFF, 1: All-Off



XT1 and YT1 are the equation variables x1(t) and y1(t):

[ 2nd ] {Y-VARS}, Y, 5: X_1T and 6: Y_1T, respectively



Example:


SEMI X-AXIS? 2

SEMI Y-AXIS? 3



Results:

APPROX. CIRC= 15.86543959

AREA= 18.84955592






TI-81 RELATIVE

Calculate the consequences of reality when it comes to a length and mass of an object traveling near the speed of light, c = 299,792,458 m/s.


Size: 141 bytes


Code:

299792458→C

Disp “C=”

Disp C

Disp “M/S”

Pause

Disp “°/. OF C”

Input P

P*C/100→U

√(1-(U/C)^2)→V

Disp “LENGTH”

Input L

Disp “OBS LENGTH=”

L*V→K

Disp K

Pause

Disp “MASS”

Input M

Disp “OBS. MASS=”

M/V→N

Disp N


Enter the percentage of the speed of light (70%, 80%, 90%, etc.). Three characters are used to create the percent sign (%) (°, / , . )


Example:


92.5% of the speed of light

length: 40.8 m

mass: 6,700 kg


Results:

observed length = 15.50265784 m

observed mass = 17,633.10542 kg


Source:


Jackson, Mark D. The QuickStudy for Physics BarCharts Publishing Inc. Boca Raton, Florida. 2007. ISBN 13: 9781423202677. pp. 114-115

Eddie


All original content copyright, © 2011-2024. Edward Shore. Unauthorized use and/or unauthorized distribution for commercial purposes without express and written permission from the author is strictly prohibited. This blog entry may be distributed for noncommercial purposes, provided that full credit is given to the author.


Sunday, October 16, 2022

TI-65: Relativity Applications

TI-65:  Relativity Applications


Introduction


The programs on today's blog entry were programmed on the Texas Instruments TI-65 calculator.   One of the features of the TI-65 is the set of physical constants.  


The programs call up the speed of light, c = 299,792,458 m/s, by the [ 3rd ] [ 2 ] key combination.  If you are using a TI-58, TI-59, or TI-66, where there are no physical constants, please store 299792458 in a memory register first, and replace the key sequence by recalling that register.  


These programs will use the shortcut:


cos(arcsin x) = √(1 - x^2) for all -1 ≤ x ≤ 1


This allows us to cut down on the number of bytes required.  


Redshift vs. Blueshift


f0 = fs * √((1 - v/c) / (1 + v/c))


v = velocity of the source/star in m/s

blueshift:  v < 0

redshift:  v > 0

fs = frequency given off by the source/star in Hz

f0 = observed frequency in Hz


v/c is stored in register 0.


Program 


Keys:

LBL F1

1

-

(

R/S

÷

[c]

)

STO 0

=

÷

(

1 

+

RCL 0

)

=

√

×

R/S

=

RTN


Key Codes:

2nd 53.53

1

49

16

51

28

3rd 46

17

12.0

39

28

16

1

59

13.0

17

39

33

38

51

39

2nd 52


Instructions:

1.  Press  [ F1 ]. 

2.  Enter v when execution stops, press [ R/S ].

3.  Enter fs when execution stops, press [ R/S ].

4.  f0 is calculated.


Example:

v = 210,000,000 m/s

fs = 450 * 10^6 Hz  (450 [ EE ] 6)

Result:  f0 = 1.888581542E8 Hz  (188.8581542 * 10^6)


Relativistic Doppler Effect


f0 = (fs * √(1 - v^2/c^2)) / (1 - v/c * cos Θ)


v = velocity of the source

Θ = direction of source's motion relative to the observer (angle from the observer's perspective)

fs = frequency given off by the source/star in Hz

f0 = observed frequency in Hz


Program


Key:

LBL F2

(

R/S

÷

[c]

)

STO 0

INV SIN

COS

×

R/S

=

÷

(

1

-

RCL 0

×

R/S

COS

)

=

RTN


Key Code:

2nd 53.54

16

51

28

3rd 46

17

12.0

-22

23

38

51

39

28

16

1

49

13.0

38

51

23

17

39

2nd 52


Instructions:

1.  Press  [ F2 ]. 

2.  Enter v when execution stops, press [ R/S ].

3.  Enter fs when execution stops, press [ R/S ].

4.  Enter Θ when the execution stops, press [ R/S ].

5.  f0 is calculated.


Example:

v = 196 * 10^6 m/s

fs = 500 * 10^6 Hz  

Θ = 40°  (degrees mode)

Result:  f0 = 7.579362482 * 10^8 Hz = 757.9362482 * 10^6 Hz


Time Dilation


t' = t0 * √(1 - (v/c)^2)


t0 = source's time 

v = velocity of source in m/s

t' = observer's time


Key:

LBL 0

R/S

÷

[ c ]

=

INV SIN

COS 

×

R/S

=

RTN


Key Codes:

2nd 53.0

51

28

3rd 46

39

-22

23

38

51

39

2nd 52


Instructions:

1.  Press  [ SBR ] [ 0 ]. 

2.  Enter v, press [ R/S ].

3.  Enter t0 when execution stops, press [ R/S ].

4.  t' is calculated.


Example:

v = 164 * 10^6 m/s

t0 = 1.5 yr

Result:  t' = 1.255654687 yr


Source:


"Sinclair Enterprise Programmable: Physics Engineering Electronics Program Library"  Sinclair Radionics Inc.  New York, NY and St. Ives, Huntingdon, Cambridgeshire UK.  1976


All original content copyright, © 2011-2022.  Edward Shore.   Unauthorized use and/or unauthorized distribution for commercial purposes without express and written permission from the author is strictly prohibited.  This blog entry may be distributed for noncommercial purposes, provided that full credit is given to the author. 

Saturday, December 6, 2014

Some Science Stocking Stuffings


Einstein's Time Dilation

Recall that equation for time dilation is:

Δt = Δt0 / √(1 - u^2/c^2)

Where:
Δt = time observed by the person standing still
Δt0 = time observed by the traveler (in the observer's frame of reference)
u = speed of the moving object , which contains the traveler
c = speed of light in a vacuum = 299,792,458 m/s

In short, the traveler will note observe and note that time Δt0 has passed, which the person standing still observes that time Δt has passed. The closer someone goes to the speed of light, that less person she/he experiences. You will need to go super fast. Driving at 65 mph (29.0756 m/s) on the freeway won't cut it and here's why:

For 1 unit of time to pass for the person driving 65 mph (Δt0 = 1), the change of time for the observer (Δt) is:

Δt = 1/√(1 - 29.0756^2/299,792,458^2) ≈ 1.0000000000000047 (that is fourteen zeroes between the decimal point and the 4) (The Wolfram Alpha app was used for this calculation).

Virtually the same time passes.

Same deal regarding observing an airplane flying at 600 mph (268.224 m/s). For the person watching the plane, for a plane's passenger, pilot, or cocktail and peanut server to observe one unit of time, us watchers observe 1.0000000000004 (twelve zeroes) units of time.

If you want to be on an object where the people observing you experience twice the time (Δt = 2) you do (Δt0 = 1), you will need to travel (c*√3)/2 or 259,627,884.491 m/s (580,771,037.247 mph). That is 86% the speed of light!

Archer's Paradox (E.J. Rendtroff, 1913)

In archery, archers aim their arrows slightly to the side, instead of directly at the target. On the surface, that seems crazy. This is where the Archer's Paradox comes into effect.

Basically, when the arrow is shot, it travels in an "S" curve. Drawing a string makes the arrow bend such that he tip is pointed away from the target. As the arrow is fired and the string returns to the bow, the arrow bends the other way, turning the arrow back to the target.

Other factors to making accurate shots include the stiffness of the arrow, brace height, and wind conditions. I found this video by Billgsgate helpful:

http://youtu.be/bNlx6MBlymw

Galactic Coordinates

Galactic Coordinates are spherical coordinates that are set such as:

* The center is our sun.
* The coordinates are (l°, b°), where l is the longitude (0° to 360°, flat angle) and the latitude (-90° to 90°, height).
* Pointing "due east", l = 0° and b = 0° is pointing towards the center of the Milky Way. "Due west", l = 180° and b = 0° points away from the center of the Galaxy.

Using Wolfram Alpha ( http://m.wolframalpha.com ) and an online coordinator converter ( http://ned.ipac.caltech.edu/forms/calculator.html ), here are the 30° longitude markers when latitude is 0° (b = 0°):

* 0° points towards the constellation Sagittarius (as it should, it having the Milky Way center)
* 30° points towards Aquila the Eagle
* 60° points towards the Vulpecula the Fox
* 90° points towards Cygnus the Swan
* 120° points towards Cassiopeia the Vain Queen
* 150° points towards Perseus the Hero
* 180° points towards Auriga the Charioteer
* 210° points towards Monoceros the Unicorn
* 240° points towards Puppis (a ship's poop deck)
* 270° points towards Vela (a ship's sails)
* 300° points towards Crux, The Southern Cross
* 330° points towards Norma (a carpenter's square (measuring tool))

Spherical Lenses (see figure 2 below)

Variables:
P = place of object (with distance s)
P' = place of image (with distance s')
C = center of curvature
V = vertex of the lens

General relations:

tan α = h/(s - δ)
tan β = h/(s' - δ)
tan Φ = h/(R - δ)

However, if α < π/2 ( α < 45° ), we are dealing with paraxial rays:

1/S + 1/S' = 2/R

Surprisingly, the object is far from the vertex.


Forgive me if I repeat things. Instead of going out to clobber everyone last Black Friday for that extra 10% off, I stayed home and cracked open some books that I have been meaning to look at for months. I hope you find this enjoyable and insightful.

The best always,

Eddie


P.S. I was thinking about adding a section (or blog entry) about the age of Aquarius and some of the head scratchers I have about it. I am not sure if this subject would be appropriate for this blog. If you have any thoughts about this, or anything else, go and ahead and comment! - E.S.



This blog is property of Edward Shore. 2014

Sharp EL-5200/EL-9000 AER II Program Collection – September 2026

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