Void Whisperer
Dark Energy Expansion Physics
Size guide S–5XL · inches
Meet the Void Whisperer, keeper of the cosmological constant Λ, the energy of empty space itself. Since 1998 we have known that the expansion of the universe is speeding up. The simplest explanation is Einstein's Λ: a constant energy density of the vacuum with equation of state w = −1, making up about 68.5% of the universe today (Planck 2018). Its density is tiny, ρ_Λ ≈ 6×10⁻²⁷ kg/m³, while a naive quantum estimate of vacuum energy comes out up to ~10¹²⁰ times too big. Why Λ is so small is unsolved: the cosmological constant problem. The Void Whisperer on a pixel-art unisex tee; equations, symbols and sources in the physics panel below.
"Empty space is never empty. Every new metre of it brings me along."
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Details
Size & fitS–5XL
Unisex heavy cotton (Gildan 5000), classic fit.
| Size | Width | Length | Sleeve |
|---|---|---|---|
| S | 18 | 28 | 15.1 |
| M | 20 | 29 | 16.5 |
| L | 22 | 30 | 18 |
| XL | 24 | 31 | 19.5 |
| 2XL | 26 | 32 | 21 |
| 3XL | 28 | 33 | 22.4 |
| 4XL | 30 | 34 | 23.7 |
| 5XL | 32 | 35 | 25 |
Ter vergelijking: maat M is 20 in (50.80 cm) breed, ongeveer 3.143 × 1034 Plancklengtes (lP = 1.616255 × 10−35 m). Een meetlint is sneller.
Measurements in inches, ±1.5 in tolerance.
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The physics
The universe's expansion is speeding up, as if empty space had its own constant energy, the cosmological constant Λ. It makes up about 68.5% of the universe today. Adding up quantum zero-point energy naively gives a value up to ~10¹²⁰ times too large, and nobody knows why the real one is so small.
Equations
| Symbol | Meaning | Unit |
|---|---|---|
| \(\Lambda\) | cosmological constant | \(\mathrm{m⁻²}\) |
| \(\rho_\Lambda\) | mass-equivalent density of the vacuum (dark) energy | \(\mathrm{kg/m³}\) |
| \(c\) | speed of light | \(\mathrm{m/s}\) |
| \(G\) | Newtonian gravitational constant | \(\mathrm{m³ kg⁻¹ s⁻²}\) |
| \(\Omega_\Lambda\) | dark-energy fraction of the critical density today, ≈ 0.685 (Planck 2018) | \(\mathrm{1}\) |
| \(H_0\) | Hubble constant, ≈ 67.4 km/s/Mpc (Planck 2018) | \(\mathrm{s⁻¹}\) |
| \(w\) | equation-of-state parameter, pressure over energy density | \(\mathrm{1}\) |
| \(p\) | pressure | \(\mathrm{Pa}\) |
| \(\bar M_{\mathrm{Pl}}\) | reduced Planck mass, ≈ 2.4×10¹⁸ GeV/c² | \(\mathrm{kg}\) |
| \(\hbar\) | reduced Planck constant | \(\mathrm{J·s}\) |
Sources
- Planck Collaboration (2020) Planck 2018 results. VI. Cosmological parameters, A&A 641, A6 (opens in a new tab)
- Weinberg (1989) The cosmological constant problem, Rev. Mod. Phys. 61, 1 (opens in a new tab)
- Riess et al. (1998) Observational Evidence from Supernovae for an Accelerating Universe, AJ 116, 1009 (opens in a new tab)
- Perlmutter et al. (1999) Measurements of Ω and Λ from 42 High-Redshift Supernovae, ApJ 517, 565 (opens in a new tab)
- NobelPrize.org — The Nobel Prize in Physics 2011 (accelerating expansion) (opens in a new tab)
- PDG 2024 review — Dark energy (opens in a new tab)
- NIST CODATA 2022 — Newtonian constant of gravitation (opens in a new tab)
Source Weinberg, S. (1989). The cosmological constant problem. Reviews of Modern Physics 61, 1–23.doi.org/10.1103/RevModPhys.61.1 (opens in a new tab)