2019A&A...632A.113D


Query : 2019A&A...632A.113D

2019A&A...632A.113D - Astronomy and Astrophysics, volume 632A, 113-113 (2019/12-0)

Circumbinary exoplanets and brown dwarfs with the Laser Interferometer Space Antenna.

DANIELSKI C., KOROL V., TAMANINI N. and ROSSI E.M.

Abstract (from CDS):


Aims. We explore the prospects for the detection of giant circumbinary exoplanets and brown dwarfs (BDs) orbiting Galactic double white dwarfs (DWDs) binaries with the Laser Interferometer Space Antenna (LISA).
Methods. By assuming an occurrence rate of 50%, motivated by white dwarf pollution observations, we built a Galactic synthetic population of P-type giant exoplanets and BDs orbiting DWDs. We carried this out by injecting different sub-stellar populations, with various mass and orbital separation characteristics, into the DWD population used in the LISA mission proposal. We then performed a Fisher matrix analysis to measure how many of these three-body systems show a periodic Doppler-shifted gravitational wave perturbation detectable by LISA.
Results. We report the number of circumbinary planets (CBPs) and BDs that can be detected by LISA for various combinations of mass and semi-major axis distributions. We identify pessimistic and optimistic scenarios corresponding, respectively, to 3 and 83 (14 and 2218) detections of CBPs (BDs), observed during the length of the nominal LISA mission. These detections are distributed all over the Galaxy following the underlying DWD distribution, and they are biased towards DWDs with higher LISA signal-to-noise ratio and shorter orbital period. Finally, we show that if LISA were to be extended for four more years, the number of systems detected will be more than doubled in both the optimistic and pessimistic scenarios.
Conclusions. Our results present promising prospects for the detection of post-main sequence exoplanets and BDs, showing that gravitational waves can prove the existence of these populations over the totality of the Milky Way. Detections by LISA will deepen our knowledge on the life of exoplanets subsequent to the most extreme evolution phases of their hosts, clarifying whether new phases of planetary formation take place later in the life of the stars. Such a method is strongly complementary to electromagnetic studies within the solar region and opens a window into the investigation of planets and BDs everywhere in the entire Galaxy, and possibly even in nearby galaxies in the Local Group.

Abstract Copyright: © C. Danielski et al. 2019

Journal keyword(s): planets and satellites: detection - brown dwarfs - white dwarfs - gravitational waves - planets and satellites: gaseous planets

Simbad objects: 19

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Number of rows : 19
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 12109 1
2 WD 0137-349 WD* 01 39 42.8531929464 -34 42 39.577891392 14.60 15.33 15.30     DA3 83 0
3 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 6567 1
4 NAME Per Arm PoG 03 30 +45.0           ~ 1434 0
5 V* UZ For CV* 03 35 28.6518733656 -25 44 21.768755424           M4.5 258 0
6 V* V471 Tau EB* 03 50 24.9666549840 +17 14 47.430910716   10.258 9.373   8.393 K2V+DA 650 0
7 V* RR Cae WD* 04 21 05.5631820426 -48 39 07.061113433 14.50 14.92 14.40     DA7.8 146 1
8 V* DP Leo CV* 11 17 15.9239894616 +17 57 41.690453220           ~ 221 1
9 LBQS 1145+0145 WD* 11 48 33.6297189672 +01 28 59.420446860           DB 170 0
10 BD-07 3477 HS* 12 44 20.2386233232 -08 40 16.846099536   10.46 10.594 10.895   sdB2VIIHe3 274 1
11 ZTF J153932.16+502738.8 WD* 15 39 32.1570293712 +50 27 38.767632120           DA 27 0
12 V* NN Ser CV* 15 52 56.1203524080 +12 54 44.429312196     16.51     DAO1+M4 261 0
13 NAME PSR B1620-26 b Pl 16 23 38.2218 -26 31 53.769           ~ 34 1
14 PSR B1620-26 Psr 16 23 38.2218 -26 31 53.769     21.30     ~ 287 2
15 KIC 10544976 ** 19 42 37.1933446896 +47 45 48.401293896   20.0   18.7   DA+M4V 15 0
16 V* HU Aqr CV* 21 07 58.1944529400 -05 17 40.557671916   16.198 15.814 14.891   D+M4V 265 1
17 V* HQ Aqr RR* 23 24 13.1765508600 -12 37 56.112134304   13.484 13.13     ~ 10 0
18 NAME Sct-Cen PoG ~ ~           ~ 195 0
19 NAME Local Group GrG ~ ~           ~ 7908 0

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2023.02.07-16:28:14

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