3.2.35 · D4 · HinglishOrbital Mechanics & Astrodynamics

ExercisesSolar radiation pressure

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3.2.35 · D4 · Physics › Orbital Mechanics & Astrodynamics › Solar radiation pressure


Level 1 — Recognition

Goal: kya tum sahi formula choose karke numbers plug in kar sakte ho? Abhi koi trap nahi.

Problem 1.1

Words aur symbols mein batao ki energy wala ek single photon kitna momentum carry karta hai, aur ek massless particle momentum carry kar bhi kyon sakta hai.

Recall Solution 1.1

WHAT: Ek photon momentum carry karta hai. WHY: Relativity deta hai . Photon ka mass hota hai, toh doosra term vanish ho jaata hai aur ho jaata hai, yaani . Purana rule sirf low-speed ke liye hai; yeh momentum ki definition nahi hai. Massless light phir bhi momentum carry karti hai kyunki momentum fundamentally energy aur flow ki direction ke baare mein hai, mass ke baare mein nahi. Dekho Photon momentum and relativity.

Problem 1.2

Sun ki luminosity hai. 1 AU par intensity compute karo aur confirm karo ki yeh quoted solar constant se match karta hai.

Recall Solution 1.2

WHAT: Power ko radius wale sphere par spread karo. WHY sphere? Energy conserved hoti hai, isliye Sun ki saari power har us sphere se pass karti hai jo Sun ke centre par centred ho (dekho Inverse-square law). Sphere ka area hota hai. Denominator: .

Problem 1.3

1 AU par ek black (absorbing) surface par base radiation pressure compute karo.

Recall Solution 1.3

WHAT: Energy flux ko se divide karke momentum flux mein convert karo. WHY: Light ka har joule momentum carry karta hai, toh momentum-per-second-per-area (= pressure) hoti hai.


Level 2 — Application

Goal: do ya teen steps chain karo, reflection aur geometry handle karo.

Problem 2.1

1000 m² area wala ek perfectly reflecting solar sail 1 AU par Sun ki taraf head-on face kar raha hai. Force nikalo.

Recall Solution 2.1

WHAT: use karo jahan (mirror), toh . WHY : Absorber momentum leta hai; mirror photon ko wapas bhejta hai momentum ke saath, toh uska momentum change hota hai. ke saath yeh factor banta hai. Chhota hai, lekin kabhi band nahi hota — mahino mein yeh bahut bada build kar leta hai (dekho Solar sails).

Problem 2.2

Wahi sail ab tilt kar di gayi hai taaki uski normal Sun ki direction se ka angle banaye. Simple model use karke force nikalo.

Recall Solution 2.2 — tilt figure dekho

Figure — Solar radiation pressure
WHAT: Sirf projected area sunlight pakadti hai. Figure dekho: incoming beam (yellow) tilted plate ko edge-on-ish dekhta hai, toh uski effective width se shrink ho jaati hai. WHY aur nahi: normal se measure hota hai (woh arrow jo plate se seedha bahar nikla ho). Jab ho toh plate Sun ki taraf fully face karti hai → full area → . Jab ho toh plate edge-on hai → kuch nahi pakadti → . Cosine woh function hai jo par aur par hota hai, toh yeh sahi tool hai. Head-on value ka exactly aadha, kyunki .

Problem 2.3

1 AU par face-on sunlight absorb karne wala ek dark asteroid chip, jiska area aur mass hai. Uska SRP acceleration nikalo.

Recall Solution 2.3

WHAT: jahan (absorber), toh . WHY se divide karo: orbits acceleration par respond karti hain, aur .


Level 3 — Analysis

Goal: scaling, ratios, aur competing effects ke baare mein reasoning karo.

Problem 3.1

Dikhao ki Mars (1.52 AU) par SRP acceleration Earth ki value ka hai, usi spacecraft ke liye.

Recall Solution 3.1

WHAT: (usi craft ke liye aur factors unchanged hain). WHY square: intensity par spread hoti hai, toh yeh ki tarah girta hai (Inverse-square law).

Problem 3.2

Explain karo, phir quantify karo, ki (SRP acceleration)/(Sun ki gravitational acceleration) ka ratio distance ke saath kyun nahi badalta, aur yeh aslal mein kya depend karta hai.

Recall Solution 3.2

WHAT: Dono accelerations likho. WHY cancel ho jaata hai: dono mein ek aakela hai. Divide karo: (aur fixed reflectivity ) ke alaawa har symbol ek universal constant hai. Toh ratio distance-independent hai lekin ke proportional hai — ek feather-light solar sail SRP strongly feel karta hai, ek dense probe barely. Isliye SRP "sirf extra gravity" nahi hai; dekho Orbital perturbations.

Problem 3.3

3.2 wale ratio ke exactly hone ke liye (SRP solar gravity ko balance kare), ek perfect absorber () ke liye kya area-to-mass ratio chahiye? use karo.

Recall Solution 3.3

WHAT: Ratio set karo aur solve karo. Numerator: . Denominator (): . Ek shocking square metres per kilogram — kisi bhi real spacecraft se bahut zyada, isliye SRP orbits ko perturb karta hai lekin ordinary craft ke liye Sun ki pull ko kabhi puri tarah cancel nahi kar sakta.


Level 4 — Synthesis

Goal: SRP ko time, momentum budgets, aur doosre perturbations ke saath combine karo.

Problem 4.1

Problem 2.1 wale 9 mN sail ka total mass hai. Yeh maante hue ki force constant rehti hai aur hamesha velocity direction mein hai, 1 year () mein gained estimate karo.

Recall Solution 4.1

WHAT: , phir (constant acceleration). WHY constant-a theek hai: 1 AU par ek year mein intensity barely badlti hai, toh ko constant treat karna ek achha first estimate hai. 9 mN ki whisper ek saal mein almost 3 km/s velocity change ban jaati hai — Solar sails ka yahi point hai: chhoti force, koi fuel nahi, enormous integrated effect.

Problem 4.2

Low Earth orbit mein ek balloon satellite dono SRP aur atmospheric drag feel karta hai. Uska SRP acceleration hai aur drag acceleration hai. (a) LEO mein kaunsa dominate karta hai? (b) Qualitatively, kis altitude par SRP drag ko overtake kar sakta hai?

Recall Solution 4.2

(a) WHAT: Magnitudes compare karo. . Drag almost zyada strong hai, toh LEO mein drag dominate karta hai. (b) WHY altitude flip karta hai: Drag air density par depend karta hai, jo altitude ke saath exponentially fall karti hai, jabki SRP altitude ke saath essentially constant hai (Sun ki distance barely badlti hai). Toh kaafi upar jao aur drag collapse kar jaata hai jabki SRP steady rehta hai — SRP kahin upper thousands of km mein drag ko overtake kar leta hai. Density model ke liye dekho Atmospheric drag.

Problem 4.3

Wavelength wala ek photon energy carry karta hai jahan . (a) Uska momentum nikalo. (b) Ek surface par 1 N force produce karne ke liye per second kitne aise photons strike karne chahiye, agar fully absorb hon?

Recall Solution 4.3

(a) WHAT: . (b) WHY: Force = momentum delivered per second = (rate ) . set karo: Ek newton ke liye almost ek trillion trillion photons per second — ek photon sach mein kuch nahi hai; barsat sab kuch hai.


Level 5 — Mastery

Goal: full mission-planner reasoning, correct physical model, saare cases.

Problem 5.1

Sun direction se angle par tilt kiye gaye perfect mirror ke liye, rigorous force plate normal ke along direct hoti hai magnitude ke saath. (a) Physically explain karo ki do cosines kahan se aate hain. (b) par ko simple-model value se compare karo.

Recall Solution 5.1 — two-cosine figure dekho

Figure — Solar radiation pressure
(a) WHY do cosines:

  • Pehla — projected area. Tilted plate beam ka sirf intercept karti hai (Problem 2.2 logic).
  • Doosra — momentum change ki direction. Mirror ke liye reflected photons normal ke baare mein symmetrically leave karte hain, toh net momentum kick normal ke along point karta hai. Incoming momentum ka sirf woh component normal ke along reverse hota hai, aur woh component full momentum times hai. Dono effects multiply karo → .

Figure dekho: blue arrow (incoming momentum) normal part (length ) aur tangential part mein split hota hai; sirf normal part reflection par reverse hota hai, green net force deta hai.

(b) Numbers (common factor drop karo; vs compare karo):

simple rigorous

par dono agree karte hain; jaise tum tilt karo, rigorous model chhota normal force deta hai. Ek sail designer jo par simple model use kare, thrust do baar over-predict karta.

Problem 5.2

Ek solar sail ko Sun ki taraf inward spiral karne ke liye "tack" karna hai. Orbital energy lose karne ke liye usse orient karna chahiye taaki SRP ka ek component uski velocity oppose kare. Agar ek perfect mirror ke liye useful along-velocity thrust component ho (normal force projected onto velocity direction), toh woh tilt angle nikalo jo ko maximise kare.

Recall Solution 5.2 — optimal tack angle figure dekho

Figure — Solar radiation pressure
WHAT tool aur WHY: Hum ki ek smooth function ka maximum chahte hain. Woh tool jo maximum dhundta hai woh derivative hai zero set karke — peak par slope flat hota hai. Define karo (constant drop karo; ek function ko scale karne se uski peak move nahi hoti). WHAT we do: differentiate karo aur zero set karo. Product rule use karo jahan aur : set karo. Solution (yaani ) edge-on hai → zero thrust, ek minimum hai, reject karo. Useful root: Figure dekho: curve badhti hai, ke paas peak karti hai, phir par zero par wapas aati hai. Ek real solar sail almost par tack karta hai, head-on nahi, apna orbit most efficiently spiral karne ke liye — ek genuine mission-design result jo tumne abhi derive kiya.


Wrap-up recall

Recall One-line takeaways (chhupao aur test karo)

Photon momentum ::: Base pressure at 1 AU ::: Simple flat-plate force ::: Rigorous mirror normal force ::: SRP/gravity distance-independent kyun hai ::: dono ; ratio Optimal solar-sail tack angle :::


Connections

  • Parent: Solar radiation pressure — woh theory jisko ye exercises drill karti hain.
  • Solar sails — Problems 4.1 aur 5.2 sail-design calculations hain.
  • Orbital perturbations — SRP ek non-gravitational perturbing force ki tarah (Problem 3.2).
  • Atmospheric drag — competing LEO force (Problem 4.2).
  • Photon momentum and relativity ki origin (Problems 1.1, 4.3).
  • Inverse-square law scaling (Problems 1.2, 3.1).
  • Yarkovsky effect — spinning asteroids par act karne wala thermal-recoil cousin.