Zobrazeno 1 - 10
of 107
pro vyhledávání: '"Andersen, Anja"'
Autor:
Konstantopoulou, Christina, De Cia, Annalisa, Ledoux, Cédric, Krogager, Jens-Kristian, Mattsson, Lars, Watson, Darach, Heintz, Kasper E., Péroux, Céline, Noterdaeme, Pasquier, Andersen, Anja C., Fynbo, Johan P. U., Jermann, Iris, Ramburuth-Hurt, Tanita
Publikováno v:
A&A 681, A64 (2024)
The evolution of the cosmic dust content and the cycle between metals and dust in the interstellar medium (ISM) play a fundamental role in galaxy evolution. The chemical enrichment of the Universe can be traced through the evolution of the dust-to-me
Externí odkaz:
http://arxiv.org/abs/2310.07709
Autor:
Konstantopoulou, Christina, De Cia, Annalisa, Krogager, Jens-Kristian, Ledoux, Cédric, Noterdaeme, Pasquier, Fynbo, Johan P. U., Heintz, Kasper E., Watson, Darach, Andersen, Anja C., Ramburuth-Hurt, Tanita, Jermann, Iris
Publikováno v:
A&A 666, A12 (2022)
Large fractions of metals are missing from the observable gas-phase in the interstellar medium (ISM) because they are incorporated into dust grains, a phenomenon called dust depletion. The study of dust depletion in the ISM is important to investigat
Externí odkaz:
http://arxiv.org/abs/2207.08804
Autor:
Nederby, Line, Trabjerg, Natacha Dencker, Andersen, Anja Bjørnskov, Lindebjerg, Jan, Hansen, Torben Frøstrup, Rahr, Hans Bjarke
Publikováno v:
In Clinical Colorectal Cancer December 2024 23(4):372-381
Autor:
Perotti, Giulia, Sørensen, Henning O., Haack, Henning, Andersen, Anja C., Sanchez, Dario Ferreira, van Kooten, Elishevah M. M. E., Tsai, Esther H. R., Dalby, Kim N., Holler, Mirko, Grolimund, Daniel, Hassenkam, Tue
Protoplanetary disks are dust- and gas-rich structures surrounding protostars. Depending on the distance from the protostar, this dust is thermally processed to different degrees and accreted to form bodies of varying chemical compositions. The primo
Externí odkaz:
http://arxiv.org/abs/2109.06942
Autor:
Watson, Darach, Hansen, Camilla J., Selsing, Jonatan, Koch, Andreas, Malesani, Daniele B., Andersen, Anja C., Fynbo, Johan P. U., Arcones, Almudena, Bauswein, Andreas, Covino, Stefano, Grado, Aniello, Heintz, Kasper E., Hunt, Leslie, Kouveliotou, Chryssa, Leloudas, Giorgos, Levan, Andrew, Mazzali, Paolo, Pian, Elena
Half of all the elements in the universe heavier than iron were created by rapid neutron capture. The theory for this astrophysical `$r$-process' was worked out six decades ago and requires an enormous neutron flux to make the bulk of these elements.
Externí odkaz:
http://arxiv.org/abs/1910.10510
Publikováno v:
A&A 624, A103 (2019)
We aim at assessing what are the most dominant dust species or types, including silicate and iron oxide grains present in the ISM, by using recent observations of dust depletion of galaxies at various evolutionary stages. We use the observed elementa
Externí odkaz:
http://arxiv.org/abs/1901.04710
The efficiency of dust formation in oxygen-rich AGB stars should (in theory) be metallicity dependent since they are not producing their own raw material for dust production. Metal-poor carbon stars may not be very efficient dust producers either, be
Externí odkaz:
http://arxiv.org/abs/1505.04811
The amount of dust estimated from infrared to sub-millimetre (submm) observations strongly depends on assumptions of different grain sizes, compositions and optical properties. Here we use a simple model of thermal emission from cold silicate/carbon
Externí odkaz:
http://arxiv.org/abs/1504.02664
Publikováno v:
A&A 568, A47 (2014)
This work presents a large consistent study of molybdenum (Mo) and ruthenium (Ru) abundances in the Milky Way. These two elements are important nucleosynthetic diagnostics. In our sample of 71 Galactic metal-poor field stars, we detect Ru and/or Mo i
Externí odkaz:
http://arxiv.org/abs/1406.6686
Recent works have demonstrated a surprisingly small variation of the dust-to-metals ratio in different environments and a correlation between dust extinction and the density of stars. Naively, one would interpret these findings as strong evidence of
Externí odkaz:
http://arxiv.org/abs/1403.0502