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Amaro Seoane P, Arca Sedda M, Babak S, Berry CPL, Berti E, Bertone G, Blas D, Bogdanović T, Bonetti M, Breivik K, Brito R, Caldwell R, Capelo PR, Caprini C, Cardoso V, Carson Z, Chen HY, Chua AJK, Dvorkin I, Haiman Z, Heisenberg L, Isi M, Karnesis N, Kavanagh BJ, Littenberg TB, Mangiagli A, Marcoccia P, Maselli A, Nardini G, Pani P, Peloso M, Pieroni M, Ricciardone A, Sesana A, Tamanini N, Toubiana A, Valiante R, Vretinaris S, Weir DJ, Yagi K, Zimmerman A. The effect of mission duration on LISA science objectives. GENERAL RELATIVITY AND GRAVITATION 2021; 54:3. [PMID: 35221342 PMCID: PMC8827205 DOI: 10.1007/s10714-021-02889-x] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 07/31/2021] [Accepted: 11/09/2021] [Indexed: 06/14/2023]
Abstract
The science objectives of the LISA mission have been defined under the implicit assumption of a 4-years continuous data stream. Based on the performance of LISA Pathfinder, it is now expected that LISA will have a duty cycle of ≈ 0.75 , which would reduce the effective span of usable data to 3 years. This paper reports the results of a study by the LISA Science Group, which was charged with assessing the additional science return of increasing the mission lifetime. We explore various observational scenarios to assess the impact of mission duration on the main science objectives of the mission. We find that the science investigations most affected by mission duration concern the search for seed black holes at cosmic dawn, as well as the study of stellar-origin black holes and of their formation channels via multi-band and multi-messenger observations. We conclude that an extension to 6 years of mission operations is recommended.
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Affiliation(s)
- Pau Amaro Seoane
- Institute of Multidisciplinary Mathematics, Universitat Politècnica de València, Valencia, Spain
- DESY Zeuthen, Zeuthen, Germany
- Institute of Applied Mathematics, Academy of Mathematics and Systems Science, CAS, Beijing, China
- Kavli Institute for Astronomy and Astrophysics, Beijing, China
| | - Manuel Arca Sedda
- Astronomisches Rechen-Institut, Zentrüm für Astronomie, Universität Heidelberg, Mönchofstr. 12-14, Heidelberg, Germany
| | - Stanislav Babak
- CNRS, Astroparticule et Cosmologie, Université de Paris, 75006 Paris, France
- Moscow Institute of Physics and Technology, Dolgoprudny, Moscow Region Russia
| | - Christopher P. L. Berry
- Department of Physics and Astronomy, Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, 1800 Sherman Ave, Evanston, IL 60201 USA
- SUPA, School of Physics and Astronomy, University of Glasgow, Kelvin Building, University Ave, Glasgow, G12 8QQ UK
| | - Emanuele Berti
- Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles St, Baltimore, MD 21218 USA
| | - Gianfranco Bertone
- Gravitation and Astroparticle Physics in Amsterdam (GRAPPA), and Institute for Theoretical Physics, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands
| | - Diego Blas
- Theoretical Particle Physics and Cosmology Group, Department of Physics, King’s College London, Strand, London, WC2R 2LS UK
- Grup de Física Teòrica, Departament de Física, Universitat Autònoma de Barcelona, 08193 Bellaterra, Spain
- Institut de Fisica d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, 08193 Bellaterra, Spain
| | - Tamara Bogdanović
- Center for Relativistic Astrophysics and School of Physics, Georgia Institute of Technology, Atlanta, GA 30332 USA
| | - Matteo Bonetti
- Università degli Studi di Milano-Bicocca, Piazza della Scienza 3, 20126 Milan, Italy
| | - Katelyn Breivik
- Center for Computational Astrophysics, Flatiron Institute, New York, NY 10010 USA
| | - Richard Brito
- CENTRA, Departamento de Física, Instituto Superior Técnico – IST, Universidade de Lisboa – UL, Avenida Rovisco Pais 1, 1049 Lisbon, Portugal
| | - Robert Caldwell
- HB6127 Wilder Lab, Department of Physics and Astronomy, Dartmouth College, Hanover, New Hampshire 03755 USA
| | - Pedro R. Capelo
- Center for Theoretical Astrophysics and Cosmology, Institute for Computational Science, University of Zurich, Winterthurerstrasse 190, 8057 Zurich, Switzerland
| | - Chiara Caprini
- Laboratoire Astroparticule et Cosmologie, CNRS UMR 7164, Université Paris-Diderot, 10 rue Alice Domon et Léonie Duquet, 75013 Paris, France
| | - Vitor Cardoso
- CENTRA, Departamento de Física, Instituto Superior Técnico – IST, Universidade de Lisboa – UL, Avenida Rovisco Pais 1, 1049 Lisbon, Portugal
| | - Zack Carson
- Department of Physics, University of Virginia, P.O. Box 400714, Charlottesville, VA 22904-4714 USA
| | - Hsin-Yu Chen
- LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139 USA
| | - Alvin J. K. Chua
- Theoretical Astrophysics Group, California Institute of Technology, Pasadena, CA 91125 USA
| | - Irina Dvorkin
- CNRS, UMR 7095, Institut d’Astrophysique de Paris, Sorbonne Université, 98 bis bd Arago, 75014 Paris, France
| | - Zoltan Haiman
- Department of Astronomy, Columbia University, 550 W. 120th St., New York, NY 10027 USA
| | - Lavinia Heisenberg
- Institute for Theoretical Physics, ETH Zurich, Wolfgang-Pauli-Strasse 27, 8093 Zurich, Switzerland
| | - Maximiliano Isi
- LIGO Laboratory, Massachusetts Institute of Technology, Cambridge, MA 02139 USA
| | - Nikolaos Karnesis
- Department of Physics, Aristotle University of Thessaloniki, 54124 Thessaloníki, Greece
- CNRS, APC, AstroParticule et Cosmologie, Université de Paris, 75013 Paris, France
| | - Bradley J. Kavanagh
- Instituto de Física de Cantabria (IFCA, UC-CSIC), Av. de Los Castros s/n, 39005 Santander, Spain
| | | | - Alberto Mangiagli
- Laboratoire Astroparticule et Cosmologie, CNRS UMR 7164, Université Paris-Diderot, 10 rue Alice Domon et Léonie Duquet, 75013 Paris, France
- Department of Physics, University of Milano - Bicocca, Piazza della Scienza 3, I20126 Milan, Italy
- National Institute of Nuclear Physics INFN, Milano - Bicocca, Piazza della Scienza 3, 20126 Milan, Italy
| | | | - Andrea Maselli
- Gran Sasso Science Institute (GSSI), 67100 L’Aquila, Italy
- Laboratori Nazionali del Gran Sasso, INFN, 67100 Assergi, Italy
| | | | - Paolo Pani
- Dipartimento di Fisica, “Sapienza” Università di Roma and Sezione INFN Roma1, Piazzale Aldo Moro 5, 00185 Rome, Italy
| | - Marco Peloso
- Dipartimento di Fisica and Astronomia, Università di Padova and Sezione INFN Padova, Via Marzolo 8, 35131 Padua, Italy
| | - Mauro Pieroni
- Blackett Laboratory, Imperial College London, London, SW7 2AZ UK
| | - Angelo Ricciardone
- 1Dipartimento di Fisica e Astronomia “G. Galilei”, Universitá degli Studi di Padova, via Marzolo 8, 35131 Padua, Italy
| | - Alberto Sesana
- Department of Physics, University of Milano - Bicocca, Piazza della Scienza 3, I20126 Milan, Italy
| | - Nicola Tamanini
- Laboratoire des 2 Infinis - Toulouse (L2IT-IN2P3), CNRS, UPS, Université de Toulouse, 31062 Toulouse Cedex 9, France
| | - Alexandre Toubiana
- CNRS, Astroparticule et Cosmologie, Université de Paris, 75006 Paris, France
- CNRS, UMR 7095, Institut d’Astrophysique de Paris, Sorbonne Université, 98 bis bd Arago, 75014 Paris, France
| | - Rosa Valiante
- INAF-Osservatorio Astronomico di Roma, via di Frascati 33, 00078 Monteporzio Catone, Italy
- INFN, Sezione di Roma I, P.le Aldo Moro 2, 00185 Rome, Italy
| | - Stamatis Vretinaris
- CNRS, APC, AstroParticule et Cosmologie, Université de Paris, 75013 Paris, France
| | - David J. Weir
- Department of Physics and Helsinki Institute of Physics, PL 64, University of Helsinki, 00014 Helsinki, Finland
- School of Physics and Astronomy, University of Nottingham, Nottingham, NG7 2RD UK
| | - Kent Yagi
- Department of Physics, University of Virginia, P.O. Box 400714, Charlottesville, VA 22904-4714 USA
| | - Aaron Zimmerman
- Center for Gravitational Physics, University of Texas at Austin, Austin, TX 78712 USA
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Sun L, Ruiz M, Shapiro SL. Simulating the magnetorotational collapse of supermassive stars: Incorporating gas pressure perturbations and different rotation profiles. PHYSICAL REVIEW. D. (2016) 2018; 98:103008. [PMID: 34589637 PMCID: PMC8477203 DOI: 10.1103/physrevd.98.103008] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
Collapsing supermassive stars (SMSs) with masses M ≳ 104-6 M ⊙ have long been speculated to be the seeds that can grow and become supermassive black holes (SMBHs). We previously performed general relativistic magnetohydrodynamic (GRMHD) simulations of marginally stable Γ = 4/3 polytropes uniformly rotating at the mass-shedding limit and endowed initially with a dynamically unimportant dipole magnetic field to model the direct collapse of SMSs. These configurations are supported entirely by thermal radiation pressure and reliably model SMSs with M ≳ 106 M ⊙. We found that around 90% of the initial stellar mass forms a spinning black hole (BH) remnant surrounded by a massive, hot, magnetized torus, which eventually launches a magnetically-driven jet. SMSs could be therefore sources of ultra-long gamma-ray bursts (ULGRBs). Here we perform GRMHD simulations of Γ ≳ 4/3, polytropes to account for the perturbative role of gas pressure in SMSs with M ≲ 106 M ⊙. We also consider different initial stellar rotation profiles. The stars are initially seeded with a dynamically weak dipole magnetic field that is either confined to the stellar interior or extended from its interior into the stellar exterior. We calculate the gravitational wave burst signal for the different cases. We find that the mass of the black hole remnant is 90%-99% of the initial stellar mass, depending sharply on Γ - 4/3 as well as on the initial stellar rotation profile. After t ~ 250-550M ≈ 1 - 2 × 103(M/106 M ⊙) s following the appearance of the BH horizon, an incipient jet is launched and it lasts for ~104-105(M/106 M ⊙) s, consistent with the duration of long gamma-ray bursts. Our numerical results suggest that the Blandford-Znajek mechanism powers the incipient jet. They are also in rough agreement with our recently proposed universal model that estimates accretion rates and electromagnetic (Poynting) luminosities that characterize magnetized BH-disk remnant systems that launch a jet. This model helps explain why the outgoing electromagnetic luminosities computed for vastly different BH-disk formation scenarios all reside within a narrow range (~1052±1 erg s-1), roughly independent of M.
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Affiliation(s)
- Lunan Sun
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Milton Ruiz
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Stuart L Shapiro
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
- Department of Astronomy & NCSA, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
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Sun L, Paschalidis V, Ruiz M, Shapiro SL. Magnetorotational collapse of supermassive stars: Black hole formation, gravitational waves, and jets. PHYSICAL REVIEW. D. (2016) 2017; 96:043006. [PMID: 30038964 PMCID: PMC6053688 DOI: 10.1103/physrevd.96.043006] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/27/2023]
Abstract
We perform magnetohydrodynamic simulations in full general relativity of uniformly rotating stars that are marginally unstable to collapse. These simulations model the direct collapse of supermassive stars (SMSs) to seed black holes that can grow to become the supermassive black holes at the centers of quasars and active galactic nuclei. They also crudely model the collapse of massive Population III stars to black holes, which could power a fraction of distant, long gamma-ray bursts. The initial stellar models we adopt are Γ = 4/3 polytropes initially with a dynamically unimportant dipole magnetic field. We treat initial magnetic-field configurations either confined to the stellar interior or extending out from the stellar interior into the exterior. We find that the black hole formed following collapse has mass MBH ≃ 0.9M (where M is the mass of the initial star) and dimensionless spin parameter aBH/MBH ≃ 0.7. A massive, hot, magnetized torus surrounds the remnant black hole. At Δt ~ 400-550M ≈ 2000 - 2700(M/106M⊙)s following the gravitational wave peak amplitude, an incipient jet is launched. The disk lifetime is Δt ~ 105(M/106M⊙)s, and the outgoing Poynting luminosity is LEM ~ 1051-52 ergs/s. If > ˜ 1 % - 10 % of this power is converted into gamma rays, Swift and Fermi could potentially detect these events out to large redshifts z ~ 20. Thus, SMSs could be sources of ultra-long gamma-ray bursts (ULGRBs), and massive Population III stars could be the progenitors that power a fraction of the long GRBs observed at redshift z ~ 5-8. Gravitational waves are copiously emitted during the collapse and peak at ~15(106M⊙/M) mHz [~0.15(104 M⊙/M) Hz], i.e., in the LISA (DECIGO/BBO) band; optimally oriented SMSs could be detectable by LISA (DECIGO/BBO) at z < ˜ 3 ( z < ˜ 11 ) .Hence, 104M⊙ SMSs collapsing at z ~ 10 are promising multimessenger sources of coincident gravitational and electromagnetic waves.
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Affiliation(s)
- Lunan Sun
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | | | - Milton Ruiz
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Stuart L Shapiro
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
- Department of Astronomy & NCSA, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
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