Why Are Pulsar Planets Rare?

Martin, Rebecca G.; Livio, Mario; Palaniswamy, Divya

doi:10.3847/0004-637x/832/2/122

Cited by 59 publications

(33 citation statements)

References 96 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Both of these arguments implicitly assume that the host is not a neutron star, which we consider to be extremely unlikely given the complete absence of easily detectable massive companions like OGLE-2016-BLG-1190Lb at a few astronomical units around pulsars. See Figure1 of Martin et al (2016) and note that while the black points have similar masses to OGLE-2016-BLG-1190Lb, they have semimajor axes a∼R e and hence are likely to be stripped stars rather than planets and, in any case, not at a∼au.…”

Section: Degeneracy Breaking From Physical Constraintsmentioning

confidence: 99%

OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

Ryu¹,

Yee²,

Udalski³

et al. 2017

View full text Add to dashboard Cite

We report the discovery of OGLE-2016-BLG-1190Lb, which is likely to be the first Spitzer microlensing planet in the Galactic bulge/bar, an assignation that can be confirmed by two epochs of high-resolution imaging of the combined source-lens baseline object. The planet's mass, M p =13.4±0.9 M J , places it right at the deuteriumburning limit, i.e., the conventional boundary between "planets" and "brown dwarfs." Its existence raises the question of whether such objects are really "planets" (formed within the disks of their hosts) or "failed stars" (lowmass objects formed by gas fragmentation). This question may ultimately be addressed by comparing disk and bulge/bar planets, which is a goal of the Spitzer microlens program. The host is a G dwarf, M host =0.89±0.07 M e , and the planet has a semimajor axis a∼2.0 au. We use Kepler K2 Campaign 9 microlensing data to break the lens-mass degeneracy that generically impacts parallax solutions from Earth-Spitzer observations alone, which is the first successful application of this approach. The microlensing data, derived primarily from near-continuous, ultradense survey observations from OGLE, MOA, and three KMTNet telescopes, contain more orbital information than for any previous microlensing planet, but not quite enough to accurately specify the full orbit. However, these data do permit the first rigorous test of microlensing orbital-motion measurements, which are typically derived from data taken over <1% of an orbital period.

show abstract

Section: Degeneracy Breaking From Physical Constraintsmentioning

confidence: 99%

OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

Ryu¹,

Yee²,

Udalski³

et al. 2017

View full text Add to dashboard Cite

show abstract

“…The pulsar timing technique has a high level of precision which allows for the detection of small, asteroid mass objects around millisecond pulsars (Thorsett & Phillips 1992;Bailes et al 1993;Blandford 1993;Wolszczan 1994Wolszczan , 1997. No asteroids have been confirmed by observations and even the detections of planets around pulsars are rare (Johnston et al 1996;Bell et al 1997;Manchester et al 2005;Kerr et al 2015;Martin et al 2016). Although, Shannon et al (2013) suggested that an asteroid belt, having a mass of about 0.05 M⊕, may be present around pulsar B1937+21.…”

Section: Introductionmentioning

confidence: 99%

Investigation of the asteroid–neutron star collision model for the repeating fast radio bursts

Smallwood

Martin

Zhang

2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The origin of fast radio bursts (FRBs) is still a mystery. One model proposed to interpret the only known repeating object, FRB 121102, is that the radio emission is generated from asteroids colliding with a highly magnetized neutron star (NS). With N -body simulations, we model a debris disc around a central star with an eccentric orbit intruding NS. As the NS approaches the first periastron passage, most of the comets are scattered away rather than being accreted by the NS. To match the observed FRB rate, the debris belt would have to be at least three orders of magnitude more dense than the Kuiper belt. We also consider the rate of collisions on to the central object but find that the density of the debris belt must be at least four orders of magnitude more dense than the Kuiper belt. These discrepancies in the density arise even if (1) one introduces a Kuiper-belt like comet belt rather than an asteroid belt and assume that comet impacts can also make FRBs; (2) the NS moves ∼ 2 orders of magnitude slower than their normal proper-motion velocity due to supernova kicks; and (3) the NS orbit is coplanar to the debris belt, which provides the highest rate of collisions.

show abstract

“…PSR 1719-14 b is a companion of the millisecond pulsar PSR J1719-1438 (spin period 5.7 ms) (Bailes et al 2011;Martin et al 2016). It has a mass of 1M jup , with an orbital period of ∼ 7837 s, and an orbital radius of 6 http://phl.upr.edu/projects/habitable-exoplanets-catalog/ top10 7 http://www.exoplaneet.info/index.html ∼ 6.6 × 10 10 cm.…”

Section: Gold Sample Objectsmentioning

confidence: 99%

“…It has a mass of 1M jup , with an orbital period of ∼ 7837 s, and an orbital radius of 6 http://phl.upr.edu/projects/habitable-exoplanets-catalog/ top10 7 http://www.exoplaneet.info/index.html ∼ 6.6 × 10 10 cm. It is identified as a planet by many researchers (Bailes et al 2011;Martin et al 2016;Spiewak et al 2018). Websites listing this object in their planet catalogues are EU, ARCHIVE, EXOKyoto, PHLUPR, and GCEXO.…”

Section: Gold Sample Objectsmentioning

confidence: 99%

Close-in Exoplanets as Candidates for Strange Quark Matter Objects

Kuerban

Geng

Huang

et al. 2020

ApJ

View full text Add to dashboard Cite

Since the true ground state of the hadrons may be strange quark matter (SQM), pulsars may actually be strange stars rather than neutron stars. According to this SQM hypothesis, strange planets can also stably exist. The density of normal matter planets can hardly be higher than 30 g cm −3 . As a result, they will be tidally disrupted when its orbital radius is less than ∼ 5.6 × 10 10 cm, or when the orbital period (P orb ) is less than ∼ 6100 s. On the contrary, a strange planet can safely survive even when it is very close to the host, due to its high density. The feature can help us identify SQM objects. In this study, we have tried to search for SQM objects among close-in exoplanets orbiting around pulsars. Encouragingly, it is found that four pulsar planets (XTE J1807-294 b, XTE J1751-305 b, PSR 0636 b, PSR J1807-2459A b) completely meet the criteria of P orb < 6100 s, and are thus good candidates for SQM planets. The orbital periods of two other planets (PSR J1719+14 b and PSR J2051-0827 b) are only slightly higher than the criteria. They could be regarded as potential candidates. Additionally, we find that the periods of five white dwarf planets (GP Com b, V396 Hya b, J1433 b, WD 0137-349 b, and SDSS J1411+2009 b) are less than 0.1 days. We argue that they might also be SQM planets. It is further found that the persistent gravitational wave emissions from at least three of these closein planetary systems are detectable to LISA. More encouragingly, the advanced LIGO and Einstein Telescope are able to detect the gravitational wave bursts produced by the merger events of such SQM planetary systems, which will provide a unique test for the SQM hypothesis.

show abstract

Why Are Pulsar Planets Rare?

Cited by 59 publications

References 96 publications

OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

Investigation of the asteroid–neutron star collision model for the repeating fast radio bursts

Close-in Exoplanets as Candidates for Strange Quark Matter Objects

Contact Info

Product

Resources

About