Question 1

When does the Sun’s declination change sign from north to south? Identify the celestial event (and zodiac reference) at which the Sun’s declination passes from positive (north) to negative (south).

Accepted Answer

Introduction / Context: The Sun’s declination varies seasonally between about +23.5° and −23.5°. The instants when declination passes through zero are the equinoxes, which also mark transitions between northern and southern declinations (and vice versa). Given Data / Assumptions: Positive declination = north of the celestial equator; negative declination = south. Vernal (March) equinox near the first point of Aries; autumnal (September) equinox near the first point of Libra. Concept / Approach: At the autumnal equinox (about September 22–23), the Sun crosses the celestial equator from north to south, so declination changes sign from positive to negative. This point corresponds to the first point of Libra in the zodiacal naming convention. Step-by-Step Solution: Identify the crossing from +δ to −δ → autumnal equinox.Match zodiac reference → first point of Libra.Therefore, both descriptions point to the same event. Verification / Alternative check: Solar ephemerides show δ = 0° and decreasing immediately after the September equinox. In March, δ crosses from negative to positive (vernal equinox, first point of Aries). Why Other Options Are Wrong: First point of Aries / vernal equinox describe the opposite transition (south to north). Autumnal equinox and first point of Libra are the correct pair. Common Pitfalls: Confusing zodiacal points Aries and Libra; remembering that Aries = March (northward), Libra = September (southward). Final Answer: Both the first point of Libra and the autumnal equinox

Question 2

Sun’s right ascension and declination – pick the comprehensive correct set Which of the following statements about the Sun’s right ascension (RA) and declination (δ) are correct?

Accepted Answer

Introduction / Context: Right ascension and declination describe the Sun’s position on the celestial sphere relative to the equator and the vernal equinox. Seasonal motion causes predictable changes in δ and steady eastward progression in RA. Given Data / Assumptions: Standard astronomical year with equinoxes near March 20–21 and September 22–23, solstices near June 21 and December 21–22. Obliquity of the ecliptic ≈ 23.5°. Concept / Approach: As Earth orbits the Sun, the apparent solar position moves along the ecliptic. RA increases continuously and wraps at 24 h near the vernal equinox direction. Declination reaches +23.5° at the June solstice, 0° at both equinoxes, and −23.5° at the December solstice. Step-by-Step Solution: (a) RA behavior: increases 0–24 h over a year → correct.(b) Maximum north declination ≈ +23.5° near June 21 → correct.(c) δ = 0° at September equinox → correct.(d) Maximum south declination ≈ −23.5° near December solstice → correct.Thus, all statements are correct. Verification / Alternative check: Almanacs and solar ephemerides list RA and δ values matching these seasonal markers. Why Other Options Are Wrong: Since (a)–(d) are all correct, any single-option choice would be incomplete; the comprehensive choice is “All of the above”. Common Pitfalls: Mixing up which equinox corresponds to northward or southward crossing; RA increases uniformly while δ oscillates between ±23.5°. Final Answer: All of the above

Question 3

On which date are both the Sun’s declination and right ascension equal to zero? Choose the correct calendar date associated with δ = 0° and RA = 0 h for the Sun.

Accepted Answer

Introduction / Context: The Sun’s equatorial coordinates provide a convenient description of seasonal changes. At the vernal equinox, the Sun crosses the celestial equator heading north and the coordinate origin is defined such that RA = 0 h at this instant. Given Data / Assumptions: Equinox dates vary slightly year to year (March 20–21 and September 22–23). At both equinoxes, solar declination δ = 0°. Concept / Approach: Although δ = 0° at both equinoxes, right ascension values differ: RA = 0 h at the vernal equinox (first point of Aries), and RA ≈ 12 h at the autumnal equinox (first point of Libra). Therefore, the unique date when both δ = 0° and RA = 0 h is the March equinox. Step-by-Step Solution: Identify the coordinate origin: first point of Aries → RA = 0 h.Match it to the calendar event: vernal equinox, about March 21.Hence choose March 21 as the correct date. Verification / Alternative check: Standard almanacs list RA(☉) ≈ 0 h at the instant of the March equinox each year, with δ ≈ 0° by definition of the celestial equator crossing. Why Other Options Are Wrong: September equinox has δ = 0° but RA ≈ 12 h, not 0 h. Solstices (June, December) have |δ| ≈ 23.5° and RA far from 0 h. Aphelion is unrelated to equatorial coordinates. Common Pitfalls: Assuming RA = 0 h at both equinoxes; only the March equinox sets the RA zero point. Final Answer: March 21 (around the vernal equinox)

Question 4

Mean scale of a vertical aerial photograph – choose the correct formula If H is the flying height above mean ground level and f is the principal distance (focal length), what is the mean scale of a true vertical photograph over plane terrain?

Accepted Answer

Introduction / Context: Scale links image measurements to ground distances. In vertical aerial photography over level ground, the mean scale is determined by the camera focal length and the aircraft height above ground at exposure. Given Data / Assumptions: True vertical photograph (zero tilt) or negligible tilt. Level terrain (no relief differences). Principal distance equals calibrated focal length f. Concept / Approach: The central projection of the camera implies that any ground distance projects to the image with a linear ratio equal to focal length over flying height. Therefore mean scale S can be written as S = image distance / ground distance = f / H, provided both are expressed in compatible units. Step-by-Step Solution: Write the basic relation for similar triangles: x / X = f / H.Recognize that scale S = x / X → S = f / H.Hence the correct expression is f / H. Verification / Alternative check: Planimetric mapping commonly assumes S = f / H for block adjustment pre-computations when relief and tilt are small. Why Other Options Are Wrong: H / f is the reciprocal (denominator of scale). (H − f) / H and H + f do not arise from the projection geometry. “None” is invalid because a standard formula exists. Common Pitfalls: Mixing up scale with the representative fraction denominator; remember RF denominator = H / f, while the scale ratio itself is f / H. Final Answer: f / H

Question 5

Distance to the horizon point on a tilted photograph On a tilted photograph with tilt angle θ, what is the distance from the principal point to the horizon point along the principal line?

Accepted Answer

Introduction / Context: Tilt introduces a visible horizon on an aerial photograph. The location of the horizon along the principal line is a key construction needed for tilt corrections and for understanding scale variations across the image. Given Data / Assumptions: Photograph of focal length f with tilt angle θ about an axis in the plate. Definitions: principal point is the perpendicular foot of the perspective center on the image plane; principal line is the line through principal and nadir/plumb points. Level terrain so the horizon is the image of the plane at infinity. Concept / Approach: For a tilted photograph, the image of the horizon lies on the principal line at a distance from the principal point given by f cot θ, measured in the direction of tilt. This follows from the perspective mapping of a horizontal plane under a rotation by θ. Step-by-Step Solution: Model the tilt as a rotation of the camera by θ.The horizon corresponds to rays parallel to the ground plane; their intercept on the image plane is at distance f cot θ.Therefore, distance PP′ (principal point to horizon point) = f cot θ along the principal line. Verification / Alternative check: Limiting cases: as θ → 0 (nearly vertical), cot θ → ∞, so the horizon recedes to infinity (not visible), which matches expectations. As θ increases, the horizon moves closer toward the principal point. Why Other Options Are Wrong: f tan θ, f sin θ, f cos θ, and f sec θ do not satisfy the correct limiting behavior and geometry of the horizon placement for small θ. Common Pitfalls: Confusing the horizon point with the isocentre or plumb point; only the horizon location follows the f cot θ relation on the principal line. Final Answer: f cot θ

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