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Searching for chameleon-like scalar fields with the ammonia method

2010/08/06 by S. A. Levshakov, A. V. Lapinov, А. В. Лапинов +5 · 3 citations
Physics and Astronomy · #Ammonia #Astro and Planetary Science #Astrophysics #Astrophysics and Star Formation Studies #Atomic physics #Context (archaeology) #Electron #Galaxy #Milky Way #Nuclear physics #Physics #Scalar (mathematics) #Stellar, planetary, and galactic studies #astro-ph.CO

paper · pdf · doi:10.1051/0004-6361/201015332

published as Astronomy & Astrophysics, v. 524, A32 (2010) · 14 pages, 5 figures, 6 tables. Accepted for publication in Astronomy and Astrophysics

arxiv created 2010/08/06 · openalex publication_date 2010/08/19 · arxiv updated 2015/06/11 · openalex created_date 2022/10/04 · openalex updated_date 2026/07/31

Abstract

Context. In our previous work we found a statistically significant offset ΔV ≈ 27 m s-1 between the radial velocities of the HC3N J = 2−1 and NH3 (J,K) = (1,1) transitions observed in molecular cores from the Milky Way. This may indicate that the electron-to-proton mass ratio, μ ≡ me/mp, increases by ~3 × 10-8 when measured under interstellar conditions with matter densities of more than 10 orders of magnitude lower than with laboratory (terrestrial) environments.

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