[HTML][HTML] H2 formation on interstellar dust grains: The viewpoints of theory, experiments, models and observations
Molecular hydrogen is the most abundant molecule in the universe. It is the first one to form
and survive photo-dissociation in tenuous environments. Its formation involves catalytic …
and survive photo-dissociation in tenuous environments. Its formation involves catalytic …
Our astrochemical heritage
P Caselli, C Ceccarelli - The Astronomy and Astrophysics Review, 2012 - Springer
Our Sun and planetary system were born about 4.5 billion years ago. How did this happen,
and what is the nature of our heritage from these early times? This review tries to address …
and what is the nature of our heritage from these early times? This review tries to address …
Cold dark clouds: the initial conditions for star formation
EA Bergin, M Tafalla - Annu. Rev. Astron. Astrophys., 2007 - annualreviews.org
Cold dark clouds are nearby members of the densest and coldest phase in the Galactic
interstellar medium, and represent the most accessible sites where stars like our Sun are …
interstellar medium, and represent the most accessible sites where stars like our Sun are …
The molecular universe
A Tielens - Reviews of Modern Physics, 2013 - APS
Molecular absorption and emission bands dominate the visible, infrared, and submillimeter
spectra of most objects with associated gas. These observations reveal a surprisingly rich …
spectra of most objects with associated gas. These observations reveal a surprisingly rich …
Chemistry of dark clouds: databases, networks, and models
The introduction of chemistry into astronomy is relatively recent and can be dated back to
about half a century ago, when molecules were discovered in space. In the 1930s it was …
about half a century ago, when molecules were discovered in space. In the 1930s it was …
CO depletion in the starless cloud core L1544
P Caselli, CM Walmsley, M Tafalla, L Dore… - The Astrophysical …, 1999 - iopscience.iop.org
We present evidence for CO depletion toward the starless cloud core L1544. A comparison
between C 17 O and the 1.3 mm continuum dust emission shows that CO is depleted by a …
between C 17 O and the 1.3 mm continuum dust emission shows that CO is depleted by a …
[HTML][HTML] Cosmic-ray ionization of molecular clouds
M Padovani, D Galli, AE Glassgold - Astronomy & Astrophysics, 2009 - aanda.org
Context. Low-energy cosmic rays are a fundamental source of ionization for molecular
clouds, influencing their chemical, thermal, and dynamical evolution. Aims. The purpose of …
clouds, influencing their chemical, thermal, and dynamical evolution. Aims. The purpose of …
[HTML][HTML] Gas phase Elemental abundances in Molecular cloudS (GEMS)-VII. Sulfur elemental abundance
Context. Gas phase Elemental abundances in molecular CloudS (GEMS) is an IRAM 30-m
Large Program aimed at determining the elemental abundances of carbon (C), oxygen (O) …
Large Program aimed at determining the elemental abundances of carbon (C), oxygen (O) …
Magnetic fields in star formation: from clouds to cores
In this chapter we review recent advances in understanding the roles that magnetic fields
play throughout the star formation process, gained through observations and simulations of …
play throughout the star formation process, gained through observations and simulations of …
Probing the evolutionary status of starless cores through N2H+ and N2D+ observations
A Crapsi, P Caselli, CM Walmsley… - The Astrophysical …, 2005 - iopscience.iop.org
We have undertaken a survey of N 2 H+ and N 2 D+ toward 31 low-mass starless cores
using the IRAM 30 m telescope. Our main objective has been to determine the abundance …
using the IRAM 30 m telescope. Our main objective has been to determine the abundance …