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Sun Data mass, m, =1.98855 - 10° kg radius, r, = 6.9634 10 m Venus Data mass, m, = 4.8675 - 10“ kg radius r, = 6.0518 - 10* m sun-venus, mean separation r = 1.08159 - 10" m orbital period, how long it takes to orbit the sun, t, = 224.701 Earth days Questions 1) Using the orbital period and the mean center to center distance of the planet from the Sun, calculate the orbital speed of Venus as it traces out its annual circle around the Sun. Select the answer that's closest to the calculation from the list below. A) 5571.14 B) 3.50205 - 10* C) 2.10027x10€ D) 1.26016x 10°: E) 3.02439 x 10° = F) 3.50045 - 10*= G) 2.97853 - 10= 2) Calculate the centripetal force necessary to hold Venus in its stable, constant- speed orbit. Enter the magnitude of the force in standard units, and do not include the unit in the answer text. Also, you can enter numbers in scientific notation using the convention that the capital letter E represents "10^," so to enter the number 1.234 × 103 you can write 1.234E23. 3) Using Newton's universal law of gravitation, calculate the magnitude of the

Sun Data mass, m, =1.98855 - 10° kg radius, r, = 6.9634 10 m Venus Data mass, m, = 4.8675 - 10“ kg radius r, = 6.0518 - 10* m sun-venus, mean separation r = 1.08159 - 10" m orbital period, how long it takes to orbit the sun, t, = 224.701 Earth days Questions 1) Using the orbital period and the mean center to center distance of the planet from the Sun, calculate the orbital speed of Venus as it traces out its annual circle around the Sun. Select the answer that's closest to the calculation from the list below. A) 5571.14 B) 3.50205 - 10* C) 2.10027x10€ D) 1.26016x 10°: E) 3.02439 x 10° = F) 3.50045 - 10*= G) 2.97853 - 10= 2) Calculate the centripetal force necessary to hold Venus in its stable, constant- speed orbit. Enter the magnitude of the force in standard units, and do not include the unit in the answer text. Also, you can enter numbers in scientific notation using the convention that the capital letter E represents "10^," so to enter the number 1.234 × 103 you can write 1.234E23. 3) Using Newton's universal law of gravitation, calculate the magnitude of the

College Physics
College Physics
11th Edition
ISBN:9781305952300
Author:Raymond A. Serway, Chris Vuille
Publisher:Raymond A. Serway, Chris Vuille
Chapter1: Units, Trigonometry. And Vectors
Section: Chapter Questions
Problem 1CQ: Estimate the order of magnitude of the length, in meters, of each of the following; (a) a mouse, (b)...
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### Sun and Venus Orbital Mechanics #### Sun Data - **Mass, \( m_s \)**: \( 1.98855 \times 10^{30} \) kg - **Radius, \( r_s \)**: \( 6.9634 \times 10^8 \) m #### Venus Data - **Mass, \( m_v \)**: \( 4.8675 \times 10^{24} \) kg - **Radius, \( r_v \)**: \( 6.0518 \times 10^6 \) m - **Sun-Venus Mean Separation, \( r_{vs} \)**: \( 1.08159 \times 10^{11} \) m - **Orbital Period, \( t_0 \)**: 224.701 Earth days #### Questions 1. **Orbital Speed Calculation** Using the orbital period and the mean center-to-center distance of the planet from the Sun, calculate the orbital speed of Venus as it traces out its annual circle around the Sun. Select the answer that’s closest to the calculation from the list below. A) 5571.14 \(\frac{m}{s}\) B) 3.52005 \(\times 10^4 \frac{m}{s}\) C) 2.10027 \(\times 10^6 \frac{m}{s}\) D) 1.26016 \(\times 10^6 \frac{m}{s}\) E) 3.02439 \(\times 10^6 \frac{m}{s}\) F) 3.50045 \(\times 10^4 \frac{m}{s}\) G) 2.97853 \(\times 10^4 \frac{m}{s}\) 2. **Centripetal Force Calculation** Calculate the centripetal force necessary to hold Venus in its stable, constant-speed orbit. Enter the magnitude of the force in standard units, and do not include the unit in the answer text. Also, you can enter numbers in scientific notation using the convention that the capital letter E represents “10^”, so to enter the number 1.234 × 10^23 you can write 1.234E23. 3. **Gr
Transcribed Image Text:### Sun and Venus Orbital Mechanics #### Sun Data - **Mass, \( m_s \)**: \( 1.98855 \times 10^{30} \) kg - **Radius, \( r_s \)**: \( 6.9634 \times 10^8 \) m #### Venus Data - **Mass, \( m_v \)**: \( 4.8675 \times 10^{24} \) kg - **Radius, \( r_v \)**: \( 6.0518 \times 10^6 \) m - **Sun-Venus Mean Separation, \( r_{vs} \)**: \( 1.08159 \times 10^{11} \) m - **Orbital Period, \( t_0 \)**: 224.701 Earth days #### Questions 1. **Orbital Speed Calculation** Using the orbital period and the mean center-to-center distance of the planet from the Sun, calculate the orbital speed of Venus as it traces out its annual circle around the Sun. Select the answer that’s closest to the calculation from the list below. A) 5571.14 \(\frac{m}{s}\) B) 3.52005 \(\times 10^4 \frac{m}{s}\) C) 2.10027 \(\times 10^6 \frac{m}{s}\) D) 1.26016 \(\times 10^6 \frac{m}{s}\) E) 3.02439 \(\times 10^6 \frac{m}{s}\) F) 3.50045 \(\times 10^4 \frac{m}{s}\) G) 2.97853 \(\times 10^4 \frac{m}{s}\) 2. **Centripetal Force Calculation** Calculate the centripetal force necessary to hold Venus in its stable, constant-speed orbit. Enter the magnitude of the force in standard units, and do not include the unit in the answer text. Also, you can enter numbers in scientific notation using the convention that the capital letter E represents “10^”, so to enter the number 1.234 × 10^23 you can write 1.234E23. 3. **Gr
### Gravitational Force Between Sun and Venus Select the best answer from the list below. A) \( 5.52234 \times 10^{2} \, \text{N} \) B) \( 5.9729 \times 10^{3} \, \text{N} \) C) \( 1.06749 \times 10^{38} \, \text{N} \) D) \( 1.76392 \times 10^{3} \, \text{N} \) E) \( 6.7785 \times 10^{2} \, \text{N} \) F) \( 7.32869 \times 10^{3} \, \text{N} \) G) \( 5.52234 \times 10^{6} \, \text{N} \) ### Problem 4: Calculate Freefall Acceleration Near Venus Calculate the acceleration a body in freefall near the surface of Venus would experience. Enter the magnitude of the acceleration in standard units, and do not include the unit in the answer text. ### Inspecting the Result of Your Calculation for Venus-Sun Gravitational Interaction: How would you expect the force the Sun exerts on Venus to change if some magical being could make the following changes to the way our solar system is configured? Anything not mentioned is assumed to remain unchanged from the original, true configuration. Select the answers to problems 5-8 from the following list of choices. A) The force increases by a factor of eight B) The force increases by a factor of three C) The force increases by a factor of two D) The force will remain unchanged E) The force decreases by a factor of two F) The force decreases by a factor of three G) The force decreases by a factor of eight ### Specific Scenarios: 5) The mass of the Sun increases by a factor of two. 6) The mass of the Sun decreases by a factor of three.
Transcribed Image Text:### Gravitational Force Between Sun and Venus Select the best answer from the list below. A) \( 5.52234 \times 10^{2} \, \text{N} \) B) \( 5.9729 \times 10^{3} \, \text{N} \) C) \( 1.06749 \times 10^{38} \, \text{N} \) D) \( 1.76392 \times 10^{3} \, \text{N} \) E) \( 6.7785 \times 10^{2} \, \text{N} \) F) \( 7.32869 \times 10^{3} \, \text{N} \) G) \( 5.52234 \times 10^{6} \, \text{N} \) ### Problem 4: Calculate Freefall Acceleration Near Venus Calculate the acceleration a body in freefall near the surface of Venus would experience. Enter the magnitude of the acceleration in standard units, and do not include the unit in the answer text. ### Inspecting the Result of Your Calculation for Venus-Sun Gravitational Interaction: How would you expect the force the Sun exerts on Venus to change if some magical being could make the following changes to the way our solar system is configured? Anything not mentioned is assumed to remain unchanged from the original, true configuration. Select the answers to problems 5-8 from the following list of choices. A) The force increases by a factor of eight B) The force increases by a factor of three C) The force increases by a factor of two D) The force will remain unchanged E) The force decreases by a factor of two F) The force decreases by a factor of three G) The force decreases by a factor of eight ### Specific Scenarios: 5) The mass of the Sun increases by a factor of two. 6) The mass of the Sun decreases by a factor of three.
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