This animation also highlights an unavoidable property of far-away events in space-time, since the direction of your world-line matters: When on your clock a far-away event happens is not set in stone until such time as light-rays from that event have the chance to reach you. As a result the readings on the far-away clocks above (on either end of the animation) depend on the assumption that the voyage will continue as planned.

The figure was drawn using Mathematica. At some point we may add code here to construct a roundtrip to any destination that you like. First, however, some notes on the relationships used are provided here.

Let's start by imagining that our traveler starts from rest at x_o=c²/α, t_o=0, and the trip is divided into quarters. The first quarter involves acceleration rightward, the second two quarters involve acceleration leftward before and after a destination event at {2x_c, 2t_c}, while the fourth involves acceleration rightward again to bring the traveler to rest back home.

First take a look the velocity-measure most simply connected to acceleration, namely hyperbolic velocity angle or rapidity η, as a function of traveler-time τ and the quarter round-trip turn-around time τ_c:

${\displaystyle \eta [\tau ]={\begin{cases}0&{\mbox{ if }}\tau \leq 0\\{\frac {\alpha \tau }{c}}&{\mbox{ if }}0<\tau \leq \tau _{c}\\{\frac {\alpha (\tau -2\tau _{c})}{c}}&{\mbox{ if }}\tau _{c}<\tau \leq 3\tau _{c}\\{\frac {\alpha (\tau -4\tau _{c})}{c}}&{\mbox{ if }}3\tau _{c}<\tau \leq 4\tau _{c}\\0&{\mbox{ if }}\tau _{c}<\tau \end{cases}}}$.

This is useful because rapidity in turn relates simply to other speed measures in (1+1)D, including proper-velocity w ≡ dx/dτ = c sinh[η], coordinate-velocity v ≡ dx/dt = c tanh[η], and Lorentz-factor γ ≡ dt/dτ = cosh[η]. Hence we can integrate them to determine map-time elapsed and distance traveled. In perhaps simplest form, the resulting integrals for each constant proper-acceleration segment may be written as:

${\displaystyle \alpha ={\frac {\Delta w}{\Delta t}}=c{\frac {\Delta \eta }{\Delta \tau }}=c^{2}{\frac {\Delta \gamma }{\Delta x}}{\text{ }}{\stackrel {v\ll c}{\rightarrow }}{\text{ }}a={\frac {\Delta v}{\Delta t}}={\frac {1}{2}}{\frac {\Delta (v^{2})}{\Delta x}}}$.

The map-trajectory for galactic-coordinates {x,t}, parameterized using traveler time τ and the quarter round-trip turn-around time τ_c, looks something like:

${\displaystyle ct[\tau ]={\begin{cases}c\tau &{\mbox{ if }}\tau \leq 0\\{\frac {c^{2}}{\alpha }}\sinh[\eta [\tau ]]&{\mbox{ if }}0<\tau \leq \tau _{c}\\2ct_{c}+{\frac {c^{2}}{\alpha }}\sinh[\eta [\tau ]]&{\mbox{ if }}\tau _{c}<\tau \leq 3\tau _{c}\\4ct_{c}+{\frac {c^{2}}{\alpha }}\sinh[\eta [\tau ]]&{\mbox{ if }}3\tau _{c}<\tau \leq 4\tau _{c}\\4c(t_{c}-\tau _{c})+c\tau &{\mbox{ if }}\tau _{c}<\tau \end{cases}}}$,

and

${\displaystyle x[\tau ]={\begin{cases}{\frac {c^{2}}{\alpha }}&{\mbox{ if }}\tau \leq 0\\{\frac {c^{2}}{\alpha }}\cosh[\eta [\tau ]]&{\mbox{ if }}0<\tau \leq \tau _{c}\\2x_{c}+{\frac {c^{2}}{\alpha }}\cosh[\eta [\tau ]]&{\mbox{ if }}\tau _{c}<\tau \leq 3\tau _{c}\\{\frac {c^{2}}{\alpha }}\cosh[\eta [\tau ]]&{\mbox{ if }}3\tau _{c}<\tau \leq 4\tau _{c}\\{\frac {c^{2}}{\alpha }}&{\mbox{ if }}\tau _{c}<\tau \end{cases}}}$.

Here t_c ≡ (c/α)sinh[ατ_c/c] and x_c ≡ (c²/α)(cosh[ατ_c/c]-1) are galactic map-coordinates for the first turn-around event at traveler-clock time τ_c. In terms of the destination distance x_d = 2x_c on the galactic map, this second equation suggests that the total roundtrip time on traveler-clocks is Δτ_round ≡ 4τ_c = 4(c/α)acosh[1+(α/c²)x_d/2]. Does that look right?

For the A and B destinations at the left and right ends (respectively) of the shuttle's oscillation, the causality limits look something like:

${\displaystyle ct_{\text{A}}[\tau ]=ct[\tau ]\pm (x[\tau ]-x[0])}$, and

${\displaystyle ct_{\text{B}}[\tau ]=ct[\tau ]\pm (x[2\tau _{c}]-x[\tau ])}$.

Of course centered in this causality-gap is the local map-time t[τ].

The tangent free-float-frame time of events for a star along our trajectory at the A and B positions may look something like:

${\displaystyle ct_{\text{A}}[\tau ]=ct[\tau ]-\tanh[\eta [\tau ]](x[\tau ]-x[0])\,}$, and

${\displaystyle ct_{\text{B}}[\tau ]=ct[\tau ]-\tanh[\eta [\tau ]](x[\tau ]-x[2\tau _{c}])\,}$.

This equation arises because -1 ≤ tanh[η] ≤ +1 is dt/dx for fixed time-isocontours associated with an extended frame of yardsticks and synchronized clocks which is moving relative to the fixed axes of an x-ct plot in flat spacetime.

We discuss these with c=1 and α=1 to minimize sprawl. In all for a constant proper-acceleration roundtrip there are four function changes, 5 intervals, and thus 5×5=25 zones involved. The plan for each of these 25 zones is to solve radar time τ[t,x] ≡ ½(τ⁺[t,x]+τ^-[t,x]) = τ_o where τ⁺[t,x] solves u=u_B[τ⁺] and τ^-[t,x] solves v=v_B[τ^-]. These in turn have been used (e.g. here) to plot radar isochrons and radar-distance grid lines for proper time/distance intervals of 0.2c²/α for all 25 zones is an x-ct diagram's field of view.

Using the linked example figure, for example working our way up from the magenta-shaded 00 zone at the bottom center of the traveler world line, we get for the radar isochrons:

${\displaystyle t_{\tau _{o}}[x]={\begin{cases}\tau _{o}&{\mbox{ in zone 00 (magenta)}}\\x\tanh[\tau _{o}]&{\mbox{ in zone 11 (blue)}}\\2\sinh[1]-(x-2\cosh[1])\tanh[\tau _{o}-2]&{\mbox{ in zone 22 (cyan)}}\\4\sinh[1]+x\tanh[\tau _{o}-4]&{\mbox{ in zone 33 (green)}}\\4\sinh[1]+\left(\tau _{o}-4\right)&{\mbox{ in zone 44 (yellow)}}\end{cases}}}$,

and for the radar-distance contours in the same zones:

${\displaystyle x_{\rho _{o}}[t]={\begin{cases}1+\rho _{o}&{\mbox{ in zone 00 (magenta)}}\\{\sqrt {e^{2\rho _{o}}+t^{2}}}&{\mbox{ in zone 11 (blue)}}\\2\cosh[1]-{\sqrt {e^{-2(\rho _{o}+2)}+(t-2\sinh[1])^{2}}}&{\mbox{ in zone 22 (cyan)}}\\{\sqrt {e^{2\rho _{o}}+\left(t-4\sinh[1]\right)^{2}}}&{\mbox{ in zone 33 (green)}}\\1+\rho _{o}&{\mbox{ in zone 44 (yellow)}}\end{cases}}}$.

To create the plot above, similar functions are needed for all 25 hk zones, where h={0,1,2,3,4} and k={0,1,2,3,4}.

The twelve zones 01, 02, 03, 10, 14, 20, 24, 30, 34, 41, 42 and 43 may require the principal value (0^th branch) of the Lambert W or product log function defined implicitly by z = We^W, namely

${\displaystyle W_{0}[x]=\sum _{n=1}^{\infty }{\frac {(-n)^{n-1}}{n!}}\ x^{n}=x-x^{2}+{\frac {3}{2}}x^{3}-{\frac {8}{3}}x^{4}+{\frac {125}{24}}x^{5}-\cdots }$

The remaining eight zones, namely 04, 12, 13, 21, 23, 31, 32, and 40, can be written out explicitly.

1. ↑ Mary Doria Russell (2008) The Sparrow (Random House, NY).
2. ↑ Carl E. Dolby and Stephen F. Gull (2001) "On radar time and the twin paradox", Amer. J. Phys. 69 (12) 1257-1261 abstract.

我，本作品的著作權持有者，決定用以下授權條款發佈本作品：

此檔案採用創用CC 姓名標示-相同方式分享 3.0 未在地化版本授權條款。

您可以自由：

• 分享 – 複製、發佈和傳播本作品
• 重新修改 – 創作演繹作品

惟需遵照下列條件：

• 姓名標示 – 您必須指名出正確的製作者，和提供授權條款的連結，以及表示是否有對內容上做出變更。您可以用任何合理的方式來行動，但不得以任何方式表明授權條款是對您許可或是由您所使用。
• 相同方式分享 – 如果您利用本素材進行再混合、轉換或創作，您必須基於如同原先的相同或兼容的條款，來分布您的貢獻成品。

https://creativecommons.org/licenses/by-sa/3.0CC BY-SA 3.0 Creative Commons Attribution-Share Alike 3.0 truetrue