The Japanese space gravitational wave antenna—DECIGO

Kawamura, Seiji; Nakamura, Takashi; Ando, Masaki; Seto, Naoki; Tsubono, K.; Numata, Kenji; Takahashi, Ryuichi; Nagano, S.; Ishikawa, Takehiko; Musha, Mitsuru; Ueda, Ken–ichi; Satō, Takashi; Hosokawa, Mizuhiko; Agatsuma, K.; Akutsu, T.; Aoyanagi, Koh-suke; Arai, K.; Araya, Akito; Asada, Hideki; Aso, Y.; Chiba, Takeshi; Ebisuzaki, Toshikazu; Eriguchi, Yoshiharu; Fujimoto, Masa–Katsu; Fukushima, Mitsuhiro; Futamase, Toshifumi; Ganzu, Katsuhiko; Harada, Tomohiro; Hashimoto, Tatsuaki; Hayama, K.; Hikida, Wataru; Himemoto, Y.; Hirabayashi, H.; Hiramatsu, Takashi; Ichiki, Kiyotomo; Ikegami, Takeshi; Inoue, Kaiki Taro; Ioka, Kunihito; Ishidoshiro, K.; Itoh, Y.; Kamagasako, S; Kanda, Nobuyuki; Kawashima, Nobuki; Kirihara, Hiroyuki; Kiuchi, Kenta; Kobayashi, S.; Kohri, Kazunori; Kojima, Yasufumi; Kokeyama, K.; Kozai, Yoshihide; Kudoh, Hideaki; Kunimori, Hiroo; Kuroda, K.; Maeda, Keiichi; Matsuhara, Hideo; Mino, Yasushi; Miyakawa, O.; Miyoki, S.; Mizusawa, Hiromi; Morisawa, Toshiyuki; Mukohyama, Shinji; Naito, Isao; Nakagawa, N.; Nakamura, Kouji; Nakano, Hiroyuki; Nakao, Ken–ichi; Nishizawa, A.; Niwa, Yasumasa; Nozawa, Choetsu; Ohashi, M.; Ohishi, N.; Ohkawa, Masashi; Okutomi, Akira; Oohara, Ken–ichi; Sago, Norichika; Saijo, Motoyuki; Sakagami, Masa–aki; Sakata, S.; Sasaki, Misao; Sato, S.; Shibata, Masaru; Shinkai, H.; Somiya, K.; Sotani, Hajime; Sugiyama, Naoshi; Tagoshi, Hideyuki; Takahashi, Tadayuki; Takahashi, Hideya; Takahashi, Ryutaro; Takano, Tadashi; Tanaka, Takahiro; Taniguchi, Keisuke; Taruya, Atsushi; Tashiro, Hiroyuki; Tokunari, Masao; Tsujikawa, Shinji; Tsunesada, Y.; Yamamoto, K.; Yamazaki, Toshitaka; Yokoyama, Jun′ichi; Yoo, Chul-Moon; Yoshida, Shijun; Yoshino, T.

doi:10.1088/0264-9381/23/8/s17

Cited by 473 publications

(331 citation statements)

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“…We refer to this nearly-spherical configuration as a Thorne-Zytkowlike object, and find this object at the end of all simulations, regardless of NS mass and pWD compaction. We find that within a radius of 100 km from the centers of mass of the remnants, K lies in the range [1,15] in cases A1, A2, and A3, ½1; 35 in case B and [1,10] in case C. Using a simple model for the temperature dependence of the specific thermal energy we estimate the characteristic temperature of these objects to be of order 10 11o K. Using a simple scaling argument [see Eq. (51)] we find that TZlO temperatures should be proportional to the compaction of the original pWD, so that in realistic WDNS head-on collisions typical remnant temperatures would be of order…”

Section: Summary and Discussionmentioning

confidence: 93%

“…If we resolve the stars adequately, the mesh size will be much smaller near the NS than near the WD, because in typical scenarios the NS is 500 times smaller than the WD. Equation (10) then implies that the smallest time step must be in the domain of the NS. In particular, if the NS is covered by N NS ¼ 2R NS =Áx NS grid zones and the WD is covered by N WD ¼ 2R WD =Áx WD grid zones, then from Eq.…”

Section: Computational Challengementioning

confidence: 99%

“…The inspiral and merger of compact binaries represent some of the most promising sources of gravitational waves (GWs) for detection by ground-based laser interferometers like LIGO [1,2], VIRGO [3,4], GEO [5], TAMA [6,7] and AIGO [8], as well as by the proposed space-based interferometers LISA [9] and DECIGO [10]. Extracting physical information from gravitational radiation emitted by compact binaries and determining their ultimate fate requires careful modeling of these systems in full general relativity (see [11] and references therein).…”

Section: Introductionmentioning

confidence: 99%

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Head-on collisions of binary white dwarf-neutron stars: Simulations in full general relativity

et al. 2011

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We simulate head-on collisions from rest at large separation of binary white dwarf-neutron stars (WDNSs) in full general relativity. Our study serves as a prelude to our analysis of the circular binary WDNS problem. We focus on compact binaries whose total mass exceeds the maximum mass that a colddegenerate star can support, and our goal is to determine the fate of such systems. A fully general relativistic hydrodynamic computation of a realistic WDNS head-on collision is prohibitive due to the large range of dynamical time scales and length scales involved. For this reason, we construct an equation of state (EOS) which captures the main physical features of neutron stars (NSs) while, at the same time, scales down the size of white dwarfs (WDs). We call these scaled-down WD models ''pseudo-WDs (pWDs).'' Using pWDs, we can study these systems via a sequence of simulations where the size of the pWD gradually increases toward the realistic case. We perform two sets of simulations; One set studies the effects of the NS mass on the final outcome, when the pWD is kept fixed. The other set studies the effect of the pWD compaction on the final outcome, when the pWD mass and the NS are kept fixed. All simulations show that after the collision, 14%-18% of the initial total rest mass escapes to infinity. All remnant masses still exceed the maximum rest mass that our cold EOS can support (1:92M ), but no case leads to prompt collapse to a black hole. This outcome arises because the final configurations are hot. All cases settle into spherical, quasiequilibrium configurations consisting of a cold NS core surrounded by a hot mantle, resembling Thorne-Zytkow objects. Extrapolating our results to realistic WD compactions, we predict that the likely outcome of a head-on collision of a realistic, massive WDNS system will be the formation of a quasiequilibrium Thorne-Zytkow-like object.

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Section: Summary and Discussionmentioning

confidence: 93%

Section: Computational Challengementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Head-on collisions of binary white dwarf-neutron stars: Simulations in full general relativity

et al. 2011

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“…In addition to the groundbased detectors, some are also considering launching detectors in space, like LISA [2] and DECIGO [3]. Since the permeability of gravitational waves could be extremely strong, one can expect to see raw information of the wave sources via gravitational waves.…”

Section: Introductionmentioning

confidence: 99%

Signatures of hadron-quark mixed phase in gravitational waves

et al. 2011

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We calculate stellar oscillations including the hadron-quark mixed phase considering the finite size effects. We find that it is possible to distinguish whether the density discontinuity exists or not in the stars, even if one will observe the gravitational waves of the fundamental mode. Additionally, the normalized eigenfrequencies of pressure modes depend strongly on the stellar mass and on the adopted equation of state. Especially, in spite of the fact that the radius of the neutron star with $1.4M_\odot$, which is standard mass, is almost independent from the equation of state with quark matter, the frequencies of pressure modes depend on the adopted equation of state. Thus, via observing the many kinds of gravitational waves, it will be possible to make a restriction on the equation of state.Comment: accepted for publication in Physical Review

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“…LISA (Laser Interferometer Space Antenna) [10] has an observation band around 1 mHz. DECIGO (DECi-hertz Interferometer Gravitational wave Observatory) [11,12] and BBO (Big Bang Observer) [13], which will be following missions of LISA, are space interferometric detectors with observation bands around 0.1 Hz. Since this band is between that of LISA and terrestrial detectors, different or complementary information on the GW sources will be obtained by DECIGO.…”

Section: Introductionmentioning

confidence: 99%

DECIGO and DECIGO pathfinder

Ando

Kawamura

Seto

et al. 2010

Class. Quantum Grav.

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A space gravitational-wave antenna, DECIGO (DECI-hertz interferometer Gravitational wave Observatory), will provide fruitful insights into the universe, particularly on the formation mechanism of supermassive black holes, dark energy and the inflation of the universe. In the current pre-conceptual design, DECIGO will be comprising four interferometer units; each interferometer unit will be formed by three drag-free spacecraft with 1000 km separation. Since DECIGO will be an extremely challenging mission with high-precision formation flight with long baseline, it is important to increase the technical feasibility before its planned launch in 2027. Thus, we are planning to launch two milestone missions. DECIGO pathfinder (DPF) is the first milestone mission, and key components for DPF are being tested on ground and in orbit. In this paper, we review the conceptual design and current status of DECIGO and DPF. PACS numbers: 04.30.Tv, 04.80.Nn, 95.55.Ym, 95.85.Sz

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The Japanese space gravitational wave antenna—DECIGO

Cited by 473 publications

References 3 publications

Head-on collisions of binary white dwarf-neutron stars: Simulations in full general relativity

Head-on collisions of binary white dwarf-neutron stars: Simulations in full general relativity

Signatures of hadron-quark mixed phase in gravitational waves

DECIGO and DECIGO pathfinder

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