BAAO 2021, Теория — Задача 2. Great Conjunctions and the Star of Bethlehem

British Astronomy and Astrophysics Olympiad 2020-2021 — Astronomy & Astrophysics Competition Paper — Saturday 27th February 2021 · 27 февруари 2021 г. · 35 т.

Указания

Time: 3 hours (∼45\sim 45 minutes for Q1, ∼65\sim 65 minutes for Q2 and ∼70\sim 70 minutes for Q3).

Questions: All three questions should be attempted. Each question contains independent parts so that later parts can be attempted even if earlier parts are incomplete.

Solutions: Answers and calculations are to be written on loose paper ON ONE SIDE ONLY. Students should ensure their name and school is clearly written on the first answer sheet and that all pages are numbered. EACH QUESTION ANSWERED must be started on a new page. A standard formula booklet with standard physical constants may be used if desired.

Instructions: This paper will be invigilated over Zoom with all candidates starting at 9am, however please do not discuss any aspect of the paper on the internet until 9am Saturday 6th^{\mathrm{th}} March.

Clarity: Solutions must be written legibly, in black pen (the papers are scanned), and working down the page. Scribble will not be marked and overall clarity is an important aspect of this exam.

Eligibility: The International Olympiad will be held during November 2021; all sixth form students are eligible to participate.

Calculators: Any standard calculator may be used, but calculators cannot be programmable and must not have symbolic algebra capability.


Training Dates and the IOAA (Bogota, Colombia, November 2021)

The team will be selected from Y12 students taking this paper as well as Y12 students taking the Senior Physics Challenge paper in March. The best students that are eligible to represent the UK at the IOAA will be invited to attend the Training Camp to be held online from (Tuesday 6th^{\mathrm{th}} April to Saturday 10th^{\mathrm{th}} April 2021). Astronomy material will be covered; problem solving skills and observational skills (telescope and naked eye observations) will be developed. At the Training Camp a Data Analysis exam along with a Round 3 theory paper will be sat. A team of five students (plus one reserve) will be selected for further training, mostly done remotely with (hopefully) additional training camps in the summer.

Important Constants
ConstantSymbolValue
Speed of lightcc3.00×108 m s−13.00\times10^{8}\ \mathrm{m\,s^{-1}}
Earth’s rotation period1 day24 hours
Earth’s orbital period1 year365.25 days
parsecpc3.09×1016 m3.09\times10^{16}\ \mathrm{m}
Astronomical Unitau1.50×1011 m1.50\times10^{11}\ \mathrm{m}
Radius of the SunR⊙R_{\odot}6.96×108 m6.96\times10^{8}\ \mathrm{m}
Radius of the EarthR⊕R_{\oplus}6.37×106 m6.37\times10^{6}\ \mathrm{m}
Mass of the SunM⊙M_{\odot}1.99×1030 kg1.99\times10^{30}\ \mathrm{kg}
Mass of the EarthM⊕M_{\oplus}5.97×1024 kg5.97\times10^{24}\ \mathrm{kg}
Luminosity of the SunL⊙L_{\odot}3.85×1026 W3.85\times10^{26}\ \mathrm{W}
Stephan-Boltzmann constantσ\sigma5.67×10−8 J m−2 K−45.67\times10^{-8}\ \mathrm{J\,m^{-2}\,K^{-4}}
Gravitational constantGG6.67×10−11 m3 kg−1 s−26.67\times10^{-11}\ \mathrm{m^{3}\,kg^{-1}\,s^{-2}}
Boltzmann constantkBk_{\mathrm{B}}1.38×10−23 J K−11.38\times10^{-23}\ \mathrm{J\,K^{-1}}
Permittivity of free spaceε0\varepsilon_08.85×10−12 F m−18.85\times10^{-12}\ \mathrm{F\,m^{-1}}
Permeability of free spaceμ0\mu_04π×10−7 H m−14\pi\times10^{-7}\ \mathrm{H\,m^{-1}}
Planck’s constanthh6.63×10−34 J s6.63\times10^{-34}\ \mathrm{J\,s}
Elementary chargeee1.60×10−19 C1.60\times10^{-19}\ \mathrm{C}
Proton rest massmpm_{\mathrm{p}}1.67×10−27 kg1.67\times10^{-27}\ \mathrm{kg}
Electron rest massmem_{\mathrm{e}}9.11×10−31 kg9.11\times10^{-31}\ \mathrm{kg}
Wien’s displacement lawλmax⁡T\lambda_{\max}T2.90×10−3 m K2.90\times10^{-3}\ \mathrm{m\,K}
Avagadro’s constantNAN_A6.02×1023 mol−16.02\times10^{23}\ \mathrm{mol^{-1}}

Basic calculus formulae:

Chain rule

ddxf(g(x))=f′(g(x))g′(x)\frac{\mathrm{d}}{\mathrm{d}x}f(g(x)) = f'(g(x))g'(x)

Product rule

ddx(uv)=dudxv+udvdx\frac{\mathrm{d}}{\mathrm{d}x}(uv) = \frac{\mathrm{d}u}{\mathrm{d}x}v + u\frac{\mathrm{d}v}{\mathrm{d}x}

Quotient rule

ddx(uv)=dudxv−udvdxv2\frac{\mathrm{d}}{\mathrm{d}x}\left(\frac{u}{v}\right) = \frac{\frac{\mathrm{d}u}{\mathrm{d}x}v - u\frac{\mathrm{d}v}{\mathrm{d}x}}{v^2}

Integration by parts

∫udvdx dx=uv−∫vdudx dx\int u\frac{\mathrm{d}v}{\mathrm{d}x}\,\mathrm{d}x = uv - \int v\frac{\mathrm{d}u}{\mathrm{d}x}\,\mathrm{d}x

Standard integral

∫1x dx=ln⁡∣x∣+C\int\frac{1}{x}\,\mathrm{d}x = \ln|x| + C
Important Formulae

You might find the diagram of an elliptical orbit below useful in solving some of the questions:

Elements of an elliptic orbit:

a=OA (=OP)a = \mathbf{OA}\ (= \mathbf{OP})semi-major axis
b=OB (=OC)b = \mathbf{OB}\ (= \mathbf{OC})semi-minor axis
e=1−b2a2e = \sqrt{1 - \frac{b^2}{a^2}}eccentricity
F\mathbf{F}focus
PF=a(1−e)\mathbf{PF} = a(1-e)periapsis distance (shortest distance from F\mathbf{F})
AF=a(1+e)\mathbf{AF} = a(1+e)apoapsis distance (longest distance from F\mathbf{F})

Kepler’s Third Law: For an elliptical orbit, the square of the period, TT, of an object about the focus is proportional to the cube of the semi-major axis, aa (as defined above), such that

T2=4π2GMa3 ,T^2 = \frac{4\pi^2}{GM}a^3\ ,

where MM is the total mass of the system (typically dominated by the central object) and GG is the universal gravitational constant.

Vis-Viva Equation: For an elliptical orbit, the speed vv of an object at a distance rr from the focus is related to the semi-major axis, aa, total mass of the system, MM, and universal gravitational constant, GG, (as defined above), such that

v2=GM(2r−1a) .v^2 = GM\left(\frac{2}{r} - \frac{1}{a}\right)\ .

Magnitudes: The apparent magnitudes of two objects, m1m_1 and m0m_0, are related to their apparent brightnesses, b1b_1 and b0b_0, via the formula

b1b0=10−0.4(m1−m0) .\frac{b_1}{b_0} = 10^{-0.4(m_1 - m_0)}\ .

The absolute magnitude of an object, M\mathcal{M}, is the same as its apparent magnitude when viewed from 10 pc, hence the relationship between apparent and absolute magnitude and distance is

m−M=5log⁡(d10) ,m - \mathcal{M} = 5\log\left(\frac{d}{10}\right)\ ,

where dd is measured in parsecs.

BAAO 2020/21 Solutions and Marking Guidelines

Note for markers:

  • Answers to two or three significant figures are generally acceptable. The solution may give more in order to make the calculation clear. Units should be present on final answers when appropriate.
  • There are multiple ways to solve some of the questions; please accept all good solutions that arrive at the correct answer. Students getting the answer in a box\boxed{\text{box}} will get all the marks available for that calculation / part of the question (as indicated in red), so long as there are no unphysical / nonsensical steps or assumptions made (students may not explicitly calculate the intermediate stages and should not be penalised for this so long as their argument is clear).

Условие

On 21st^{\mathrm{st}} December 2020, Jupiter and Saturn formed a true spectacle in the southwestern sky just after sunset in the UK, separated by only 0.102∘0.102^{\circ}. This is close enough that when viewed through a telescope both planets and their moons could be seen in the same field of view (see Fig 4).

When two planets occupy the same piece of sky it is known as a conjunction, and when it is Jupiter and Saturn it is known as a great conjunction (so named because they are the rarest of the naked-eye planet conjunctions). The reason it happens is because Jupiter’s orbital velocity is higher than Saturn’s and so as time goes on Jupiter catches up with and overtakes Saturn (at least as viewed from Earth), with the moment of overtaking corresponding to the conjunction. The process of the two getting closer and closer together has been seen in sky throughout the year (see Fig 5).

Left: telescope image on a blue twilight sky labelled '16:30 UTC, 20 December 2020' showing Saturn with moons Rhea and Titan above, and Jupiter with Callisto, Ganymede, Io and Europa below, plus the star HD191250. Right: black-background telescope image with ringed Saturn at the top and banded Jupiter with faint moons at the bottom.
Figure 4: Left: The view of the planets the day before their closest approach, as captured by the 16” telescope at the Institute of Astronomy, Cambridge. Credit: Robin Catchpole. Right: The view from Arizona on the day of the closest approach as viewed with the Lowell Discovery Telescope. Credit: Levine / Elbert / Bosh / Lowell Observatory.

a. (i) In ideal observing conditions the two planets are far enough apart that they should be (just about) distinguishable to the naked eye, however to some observers in imperfect conditions they would appear as a single bright dot, brighter than either planet on its own.

During the conjunction, the apparent magnitudes of Jupiter and Saturn were mJ=−1.97m_J = -1.97 and mS=0.63m_S = 0.63, respectively (ignoring dimming by the atmosphere). What would be the apparent magnitude of the two planets if they appeared to an observer as a single point? [Hint: it is not simply −1.97−0.63=−2.60-1.97 - 0.63 = -2.60.] [3 т.]

a. (ii) Although they appeared close in angle, there was a very considerable distance between the two planets. At conjunction, Jupiter was 5.9265.926 au from Earth whilst Saturn was 10.82710.827 au (see Fig 5). If they were actually next to each other in space such that they could be treated as a single object, how far from the Earth (in au) would they need to be to have the same apparent magnitude as calculated in the previous part? For simplicity, assume that both planets can be modelled as (very low luminosity) stars so that the change in brightness is only due to changing the distance from the Earth (i.e. ignore the complications from the changing distance from the Sun affecting the number of reflected photons and the changing geometry affecting the illuminated fraction of the planet’s surface). [3 т.]

Left: composite over a sunset horizon of the positions of Saturn (left column) and Jupiter (right column) joined by lines on dates from 02 Oct 2020 (7° 19′) to 21 Dec 2020 (0° 06′), every five days. Right: diagram of orbits with Saturn, Jupiter, the Sun and Earth, a dashed line of sight from Earth through Jupiter to Saturn, labelled 'Great Conjunction 2020'.
Figure 5: Left: Demonstrating how Jupiter and Saturn have been getting closer and closer together over the last few months. Separations are given in degrees and arcminutes (1/60th1/60^{\mathrm{th}} of a degree). Credit: Pete Lawrence. Right: The positions of the Earth, Jupiter and Saturn that were responsible for the 2020 great conjunction. The precise timing of the apparent alignment is clearly sensitive to where Earth is in its orbit. Credit: timeanddate.com.

The time between conjunctions is known as the synodic period. Although this period will change slightly from conjunction to conjunction due to different lines of perspective as viewed from Earth (see Fig 5), we can work out the average time between great conjunctions by considering both planets travelling on circular coplanar orbits and ignoring the position of the Earth.

b. (i) Jupiter has a period of 4332.5894332.589 days and Saturn has a period of 10 759.2210\,759.22 days (where 11 day =24= 24 hours). Note: be careful as your calculations will be very sensitive to rounding errors.

Calculate the time between great conjunctions as viewed from the centre of the Solar System (this will be equal to the average synodic period). Give your answer in years (where 11 year =365.25= 365.25 days). [Hint: consider a reference frame rotating at the same rate as Jupiter.] [2 т.]

b. (ii) Use your answer to predict the date (to the nearest day) of the next great conjunction. [3 т.]

b. (iii) Some astronomers have suggested that the ‘Star of Bethlehem’ seen by the magi (‘wise men’) on their way to Jesus’ birth was in fact a great conjunction. Use your average synodic period to find the date of the great conjunction in the first decade BC and give your answer to the nearest month. [Note: be careful with BC years as year 0 in your calculation is equivalent to 1 BC, since 31st^{\mathrm{st}} December 1 BC is followed by 1st^{\mathrm{st}} January 1 AD] [5 т.]

For circular coplanar orbits the centre of Jupiter’s disc would pass in front of the centre of Saturn’s disc every conjunction, and hence have an angular separation of θ=0∘\theta = 0^{\circ} (it is measured from the centre of each disc). In practice, the planets follow elliptical orbits that are in planes inclined at different angles to each other.

Fig 6 shows how this affects the real values for over 8000 years’ worth of data, which along with different synodic periods between conjunctions makes it a difficult problem to solve precisely without a computer. However, after one synodic period Saturn has moved about 2/32/3 of the way around its orbit, and so roughly every 33 synodic periods it is in a similar part of the sky. Consequently every third great conjunction follows a reasonably regular pattern which can be fit with a sinusoidal function.

c. (i) By empirically fitting a sinusoidal function (which is assumed to be the same for each track, just with a fixed phase difference between them) and assuming all conjunctions are separated by the average synodic period, we can give rough estimations for the separations of any given great conjunction. Note: be careful as your calculations will be very sensitive to rounding errors.

By reading off the graph, give an equation for Track A of the form θ=∣Dsin⁡(2πtλ+ϕA)∣\theta = |D\sin(\frac{2\pi t}{\lambda} + \phi_A)|, where tt is the (decimalised) date in years, and DD, λ\lambda, and −π/2<ϕA≤π/2-\pi/2 < \phi_A \leq \pi/2 are values that need to be determined. [Hint: ensure your function passes through the 2020 data point, and the function is decreasing as it does.] [4 т.]

c. (ii) Without having to read anything else off the graph, write down the equations for Tracks B and C, given the same restrictions on ϕB\phi_B and ϕC\phi_C. [3 т.]

c. (iii) State which track the ‘Star of Bethlehem’ great conjunction is on, and hence use the relevant equation to predict its separation. How does it compare to the 2020 great conjunction? [3 т.]

c. (iv) When is the next great conjunction at least as close as the 2020 one (i.e. θ≤0.102∘\theta \leq 0.102^{\circ})? Give its year and the value of θ\theta. [2 т.]

c. (v) Similarly, when was the last great conjunction at least as close as the 2020 one? Give its year and the value of θ\theta. [4 т.]

c. (vi) Using your equations, calculate the probability that a great conjunction has θ≤0.102∘\theta \leq 0.102^{\circ}. [3 т.]

Top: scatter plot of separation (°) from 0 to 1.2 versus year from 1800 to 2300 for Track A (orange circles), Track B (green squares) and Track C (blue triangles); the orange point at about 0.10° in 2020 is annotated '21 Dec. 2020 Great Conjunction', with a dashed line at 0. Bottom: the same three tracks from about 1600 to 10000 (axis 'Year'), separation 0.00 to 1.25, forming interleaved sinusoidal patterns with points of varying opacity.
Figure 6: Top: All great conjunctions from 1800 to 2300, calculated for the real celestial mechanics of the Solar System. We can see that each great conjunction belongs to one of three different series or tracks, with Track A indicated with orange circles, Track B with green squares, and Track C with blue triangles. Bottom: The same idea but extended over a much larger date range, up to 10 000 AD. It is clear the distinct series form broadly sinusoidal patterns which can be used with the average synodic period to give rough predictions for the separations of great conjunctions. The opacity of points is related to each conjunction’s angular separation from the Sun (where low opacity means close to the Sun, so it is harder for any observers to see). Credit: Nick Koukoufilippas, but inspired by the work of Steffen Thorsen and Graham Jones / Sky & Telescope.

Отговори

Решение

END OF PAPER

END OF PAPER

Questions proposed by:
Dr Alex Calverley (Royal Grammar School, Guildford)
Niam Vaishnav (University of Oxford)
Nick Koukoufilippas (University of Oxford)


Оригинал в Архива: BAAO_2021.pdf · официални решения: BAAO_2021_solutions.pdf