Skip to main content

Special Relativity

  • Chapter
  • First Online:
Introduction to General Relativity

Part of the book series: Undergraduate Lecture Notes in Physics ((ULNP))

  • 147k Accesses

Abstract

We introduce the theory of special relativity, namely the theoretical framework based on the Einstein Principle of Relativity. In Newtonian mechanics, we have space and time as two distinct entities and time is the same for all observers. Such a set-up breaks down when we impose that interactions do not propagate instantaneously with infinite velocity (an implicit assumption in the theory of Galilean relativity). In special relativity we have spacetime as the natural stage for the description of physical phenomena.

This is a preview of subscription content, log in via an institution to check access.

Access this chapter

Chapter
USD 29.95
Price excludes VAT (USA)
  • Available as PDF
  • Read on any device
  • Instant download
  • Own it forever
eBook
USD 54.99
Price excludes VAT (USA)
  • Available as EPUB and PDF
  • Read on any device
  • Instant download
  • Own it forever
Softcover Book
USD 69.99
Price excludes VAT (USA)
  • Compact, lightweight edition
  • Dispatched in 3 to 5 business days
  • Free shipping worldwide - see info

Tax calculation will be finalised at checkout

Purchases are for personal use only

Institutional subscriptions

Notes

  1. 1.

    Some authors use a different convention. For an (\(n+1\))-dimensional spacetime (n spatial dimensions \(+\) 1 temporal dimension), they write the coordinates of the spacetime as \((x^1,x^2, \ldots , x^{n+1})\), where \(x^{n+1}\) is the time coordinate. In such a case, the Minkowski metric in Eq. (2.9) becomes \(\eta _{\mu \nu } = \mathrm{diag} (1,1, \ldots , 1,-1)\).

  2. 2.

    The convention of a metric with signature \((-+++)\) is common in the gravity community. In the particle physics community it is more common the convention of a metric with signature \((+---)\).

  3. 3.

    Throughout the book, we use Latin letters \(i,j, k, \ldots \) for space indices (\(1,2, \ldots , n\)), where n is the number of spatial dimensions, and Greek letters \(\mu ,\nu ,\rho , \ldots \) for spacetimes indices (\(0, 1, 2, \ldots , n\)). Such a convention is also used when we sum over repeated indices. For instance, for \(n=3\) we have

    figure a

    If we wrote \(\eta _{ij} dx^j dx^i\), we would mean

    figure b

    because i and j can run from 1 to n.

  4. 4.

    With the convention \(\eta _{\mu \nu } = \mathrm{diag}(1,-1,-1,-1)\) common in particle physics, the line element along particle trajectories is \(ds^2 > 0\) (\(ds^2 < 0\)) if the particle moves at a speed lower (higher) than c. In that context, time-like curves have \(ds^2 > 0\) and space-like curves have \(ds^2 < 0\).

  5. 5.

    Note the difference of the position of the indices \(\mu \) and \(\nu \) in \(\varLambda ^\mu _{\nu }\) and \(\varLambda _\mu ^{\nu }\). Indeed

    figure c

    However, since the matrices of the Lorentz transformations are symmetric, sometimes the notation \(\varLambda ^\mu _\nu \) and \(\varLambda _\mu ^\nu \) is used when it is clear the initial and the final coordinate systems.

  6. 6.

    As we will see in Sect. 6.6, there is also a contribution of opposite sign due to the difference in the gravitational field between the two points.

Author information

Authors and Affiliations

Authors

Corresponding author

Correspondence to Cosimo Bambi .

Problems

Problems

2.1

The energy-momentum tensor of a perfect fluid in Cartesian coordinates and in the rest-frame of the fluid has the following form

$$\begin{aligned} || T^{\mu \nu } || = \left( \begin{array}{cccc} \varepsilon &{} 0 &{} 0 &{} 0 \\ 0 &{} P &{} 0 &{} 0 \\ 0 &{} 0 &{} P &{} 0 \\ 0 &{} 0 &{} 0 &{} P \\ \end{array} \right) \, , \end{aligned}$$
(2.60)

where \(\varepsilon \) and P are, respectively, the energy density and the pressure of the fluid. Write \(T^{\mu \nu }\), \(T^{\mu }_{\nu }\), and \(T_{\mu \nu }\) in spherical coordinates.

2.2

Consider the coordinate transformation \(x^\mu \rightarrow x'^\mu \) in Eq. (2.28). Write the energy-momentum tensor of a perfect fluid in Eq. (2.60) in the new reference frame moving with velocity v along the x axis.

2.3

Let us consider three inertial reference frames with, respectively, Cartesian coordinates (ctxyz), \((ct',x',y', z')\), and \((ct'',x'',y'', z'')\). The reference frame \((ct',x',y', z')\) moves with the velocity \(\mathbf{v} = (v, 0,0)\) with respect to the reference frame (ctxyz), and the reference frame \((ct'',x'',y'', z'')\) moves with the velocity \(\mathbf{v}' = (v', 0,0)\) with respect to the reference frame \((ct',x',y', z')\). For \(t = t' = t'' = 0\) the three reference frames coincide. Write the Lorentz boost connecting the reference frames (ctxyz) and \((ct'',x'',y'', z'')\).

2.4

Show that Lorentz transformations do not commute in general.

2.5

The GPS Navigation System consists of a network of satellites in high orbits around Earth. Each satellite has an orbital speed of about 14,000 km/hour. What is the relation between the time measured by a clock on one of these satellites and by a clock on Earth due to the orbital motion of the satellite?Footnote 6

Rights and permissions

Reprints and permissions

Copyright information

© 2018 Springer Nature Singapore Pte Ltd.

About this chapter

Check for updates. Verify currency and authenticity via CrossMark

Cite this chapter

Bambi, C. (2018). Special Relativity. In: Introduction to General Relativity. Undergraduate Lecture Notes in Physics. Springer, Singapore. https://doi.org/10.1007/978-981-13-1090-4_2

Download citation

Publish with us

Policies and ethics