Zobrazeno 1 - 10
of 73
pro vyhledávání: '"Rastello, Sara"'
Autor:
Iorio, Giuliano, Torniamenti, Stefano, Mapelli, Michela, Dall'Amico, Marco, Trani, Alessandro A., Rastello, Sara, Sgalletta, Cecilia, Rinaldi, Stefano, Costa, Guglielmo, Dhal-Lahtinen, Bera A., Escobar, Gaston J., Korb, Erika, Vaccaro, M. Paola, Lacchin, Elena, Mestichelli, Benedetta, di Carlo, Ugo Niccolò, Spera, Mario, Sedda, Manuel Arca
Gaia BH3 is the first observed dormant black hole (BH) with a mass of $\approx{30}$ M$_\odot$ and represents the first confirmation that such massive BHs are associated with metal-poor stars. Here, we explore the isolated binary formation channel for
Externí odkaz:
http://arxiv.org/abs/2404.17568
Autor:
Pina, Daniel Marín, Rastello, Sara, Gieles, Mark, Kremer, Kyle, Fitzgerald, Laura, Forastier, Bruno Rando
Publikováno v:
A&A 688, L2 (2024)
Context. The star-black hole (S-BH) binary known as Gaia BH3, discovered by the Gaia Collaboration is chemically and kinematically associated with the metal-poor ED-2 stream in the Milky Way halo. Aims. We explore the possibility that Gaia BH3 was as
Externí odkaz:
http://arxiv.org/abs/2404.13036
Autor:
Sedda, Manuel Arca, Kamlah, Albrecht W. H., Spurzem, Rainer, Giersz, Mirek, Berczik, Peter, Rastello, Sara, Iorio, Giuliano, Mapelli, Michela, Gatto, Massimiliano, Grebel, Eva K.
We present the first results of the \textsc{Dragon-II} simulations, a suite of 19 $N$-body simulations of star clusters with up to $10^6$ stars, with up to $33\%$ of them initially paired in binaries. In this work, we describe the main evolution of t
Externí odkaz:
http://arxiv.org/abs/2307.04805
Autor:
Rastello, Sara, Iorio, Giuliano, Mapelli, Michela, Arca-Sedda, Manuel, Di Carlo, Ugo N., Escobar, Gastón J., Torniamenti, Stefano, Shenar, Tomer
$Gaia$ BH1, the first quiescent black hole (BH) detected from $Gaia$ data, poses a challenge to most binary evolution models: its current mass ratio is $\approx{0.1}$, and its orbital period seems to be too long for a post-common envelope system and
Externí odkaz:
http://arxiv.org/abs/2306.14679
Autor:
Torniamenti, Stefano, Rastello, Sara, Mapelli, Michela, Di Carlo, Ugo N., Ballone, Alessandro, Pasquato, Mario
Dynamical interactions in dense star clusters are considered one of the most effective formation channels of binary black holes (BBHs). Here, we present direct $N-$body simulations of two different star cluster families: low-mass ($\sim{500-800}$ M$_
Externí odkaz:
http://arxiv.org/abs/2203.08163
Autor:
Périgois, Carole, Santoliquido, Filippo, Bouffanais, Yann, Di Carlo, Ugo N., Giacobbo, Nicola, Rastello, Sara, Mapelli, Michela, Regimbau, Tania
We study the impact of young clusters on the gravitational wave background from compact binary coalescence. We simulate a catalog of sources from population I/II isolated binary stars and stars born in young clusters, corresponding to one year of obs
Externí odkaz:
http://arxiv.org/abs/2112.01119
Autor:
Trani, Alessandro Alberto, Rastello, Sara, Di Carlo, Ugo N., Santoliquido, Filippo, Tanikawa, Ataru, Mapelli, Michela
A binary star orbited by an outer companion constitutes a hierarchical triple system. The outer body may excite the eccentricity of the inner binary through the von~Zeipel-Lidov-Kozai (ZLK) mechanism, triggering the gravitational wave (GW) coalescenc
Externí odkaz:
http://arxiv.org/abs/2111.06388
Autor:
Dall'Amico, Marco, Mapelli, Michela, Di Carlo, Ugo N., Bouffanais, Yann, Rastello, Sara, Santoliquido, Filippo, Ballone, Alessandro, Sedda, Manuel Arca
Publikováno v:
Monthly Notices of the Royal Astronomical Society, Volume 508, Issue 2, December 2021, Page 3045
GW190521 is the most massive binary black hole (BBH) merger observed to date, and its primary component lies in the pair-instability (PI) mass gap. Here, we investigate the formation of GW190521-like systems via three-body encounters in young massive
Externí odkaz:
http://arxiv.org/abs/2105.12757
Autor:
Rastello, Sara, Mapelli, Michela, di Carlo, Ugo N., Iorio, Giuliano, Ballone, Alessandro, Giacobbo, Nicola, Santoliquido, Filippo, Torniamenti, Stefano
Young star clusters are dynamically active stellar systems and are a common birthplace for massive stars. Low-mass star clusters ($\sim{}300-10^3$ M$_\odot$) are more numerous than massive systems and are characterized by a two-body relaxation time s
Externí odkaz:
http://arxiv.org/abs/2105.01669
Autor:
Di Carlo, Ugo N., Mapelli, Michela, Pasquato, Mario, Rastello, Sara, Ballone, Alessandro, Dall'Amico, Marco, Giacobbo, Nicola, Iorio, Giuliano, Spera, Mario, Torniamenti, Stefano, Haardt, Francesco
Intermediate mass black holes (IMBHs) in the mass range $10^2-10^5\,\mathrm{M_{\odot}}$ bridge the gap between stellar black holes (BHs) and supermassive BHs. Here, we investigate the possibility that IMBHs form in young star clusters via runaway col
Externí odkaz:
http://arxiv.org/abs/2105.01085