⚛️ Physics Simulation Lab
Six interactive simulations covering core high school physics — adjust parameters and watch the physics happen in real time.
⚙️ Parameters
Initial Speed (m/s) 25
Launch Angle (°) 45
Gravity (m/s²) 9.81
Air Resistance None
0 m
Range
0 m
Max Height
0 s
Flight Time
0 m/s
Vₓ (now)
🖼 Trajectory
📐 Equations
x(t) = v₀·cos(θ)·t
y(t) = v₀·sin(θ)·t − ½·g·t²
Range R = v₀²·sin(2θ) / g
H_max = v₀²·sin²(θ) / (2g)
Key insight: Maximum range at 45°. Complementary angles (e.g. 30° and 60°) give the same range but different flight times and heights.
⚙️ Parameters
Length (m) 1.0
Initial Angle (°) 20
Gravity (m/s²) 9.81
Damping Low
0 s
Period T
0 Hz
Frequency f
0 J
Kinetic Energy
0 J
Potential Energy
🖼 Pendulum + Energy Graph
📐 Equations
T = 2π·√(L/g)
θ''(t) = −(g/L)·sin(θ)
KE = ½·m·v² PE = m·g·h
Key insight: Period depends only on length and gravity — not mass or amplitude (for small angles). Doubling the length multiplies T by √2 ≈ 1.41.
⚙️ Wave 1
Amplitude A₁ 1.0
Frequency f₁ (Hz) 1.0
⚙️ Wave 2
Amplitude A₂ 1.0
Frequency f₂ (Hz) 1.0
Phase Δφ (°) 0
—
Beat Freq.
—
Interference
🖼 Wave Superposition
📐 Equations
y₁ = A₁·sin(2πf₁t + φ₁)
y₂ = A₂·sin(2πf₂t + φ₂)
y = y₁ + y₂ (superposition)
f_beat = |f₁ − f₂|
Try: Set f₁=1, f₂=1, Δφ=0 → constructive. Δφ=180° → destructive. Set f₁≠f₂ → beats.
⚙️ Circuit
Type
Voltage V (V) 12
R₁ (Ω) 10
R₂ (Ω) 20
R₃ (Ω) 30
0 Ω
R_total
0 A
I_total
0 W
P_total
0 V
V across R₁
🖼 Circuit Diagram (live current animation)
📐 Ohm's Law & Power
V = I·R → I = V/R
R_series = R₁ + R₂ + R₃
1/R_parallel = 1/R₁ + 1/R₂ + 1/R₃
P = V·I = I²·R = V²/R
Key insight: In series circuits, current is the same everywhere but voltage divides. In parallel, voltage is the same but current divides.
⚙️ Lens Settings
Lens Type
Focal Length f (cm) 10
Object Distance u (cm) 25
Object Height h (cm) 4
— cm
Image distance v
—×
Magnification
—
Image type
— cm
Image height
🖼 Ray Diagram
📐 Lens Equation
1/f = 1/v + 1/u
m = −v/u = h_i / h_o
Conventions: Object on left (u +ve). Real image: v +ve, on right. Virtual image: v −ve, same side as object. m > 0 upright, m < 0 inverted.
⚙️ Orbital Mechanics
Central Mass M 1.0×
Orbital Radius r 150
Planet Mass m 1.0×
Eccentricity 0.00
— s
Period T
— km/s
Orbital speed
—
KE (rel.)
—
PE (rel.)
🖼 Orbital Simulation
📐 Kepler + Newton
F = GMm/r² (Newton's Law)
v_orb = √(GM/r)
T² ∝ r³ (Kepler's 3rd Law)
Key insight: Increase eccentricity to see Kepler's 2nd Law in action — the planet sweeps equal areas in equal times (moves faster near the star).
