Wednesday, November 11, 2015

A System of Five Super-Earths and a Saturn-Mass Planet

Vogt et al. (2015) present the discovery of a six-planet system orbiting the nearby K3V star HD 219134. The planetary system consists of at least 5 super-Earth mass planets in a compact configuration and a Saturn-mass planet orbiting much further out. The six planets have orbital periods of 3.1, 6.8, 22.8, 46.7, 94.2 and 2247 days, spanning 3.8, 3.5, 8.9, 21.3, 10.8 and 108 times the Earth’s mass, respectively. All 5 inner planets orbit HD 219134 closer than Mercury’s average distance from the Sun.

The six planets around HD 219134 were detected by precisely measuring the tiny wobbles the planets induce on their host star. The 5 inner planets are orbiting too close, and hence, too hot to be habitable. Nevertheless, HD 219134 is 0.31 times as luminous as the Sun and a planet orbiting it at 0.56 AU, corresponding to an orbital period of 167 days, would receive the same intensity of stellar radiation Earth receives from the Sun. If this hypothetical planet has a mass equal to that of Earth, the amount of wobbling it induces on its host star would be challenging but not impossible to detect.

Vogt et al. (2015), “A Six-Planet System Orbiting HD 219134”, arXiv:1509.07912 [astro-ph.EP]

Tuesday, November 10, 2015

Giant Planet Transiting a Rapidly Rotating A-Type Star

HAT-P-57b is a giant planet in a close-in orbit around a rapidly rotating A8V star. A-type stars are more massive and much more luminous than F, G and K-type stars. To date, only a handful of planets have been found around A-type stars. HAT-P-57b was detectable because it transits its host star every 2.465 days, which is also the orbital period of the planet around its host star. Such a short orbital period implies HAT-P-57b is in an extremely close-in orbit, only about 5 stellar radii from the surface of its host star. HAT-P-57b is estimated to have an equilibrium temperature of roughly 2200 K.

The host star of is estimated to have 1.47 ± 0.12 times the mass, 1.500 ± 0.050 times the radius and 6.4 ± 1.1 times the luminosity of the Sun. With an equatorial rotation velocity of at least 102 km/s, the host star of HAT-P-57b has the highest rotation velocity of any star currently known to host a transiting planet. The next most rapidly rotating stars to host transiting planets are KOI-89 with a rotation velocity of at least 90 km/s and WASP-33 with a rotation velocity of at least 86 km/s. Finally, the mass of HAT-P-57b is estimated to be no more than 1.85 times the mass of Jupiter.

Transit light curve indicating the presence of HAT-P-57b. Hartman et al. (2015)

Hartman et al. (2015), “HAT-P-57b: A Short-Period Giant Planet Transiting A Bright Rapidly Rotating A8V Star Confirmed Via Doppler Tomography”, arXiv:1510.08839 [astro-ph.EP]

Thursday, September 10, 2015

Discovery of the Least Massive Quadruple System

2M0441+2301 AabBab is a quadruple system comprised of two pairs of binary objects with a projected separation of about 1,800 AU between them. The more massive binary system, 2M0441+2301 Aab, consists of a low-mass star (the "Aa" component) and a brown dwarf companion (the "Ab" component) 33 AU away. The less massive binary system, 2M0441+2301 Bab, consists of a brown dwarf (the "Ba" component) and a planetary-mass companion (the "Bb" component) 15 AU away. Mass estimates indicate Aa has 200 times Jupiter's mass, Ab has 35 times Jupiter's mass, Ba has 19 times Jupiter's mass and Bb has 9.8 times Jupiter's mass. 2M0441+2301 AabBab is currently the least massive quadruple system known.

Figure 1: Artist’s impression of a multiple system.

2M0441+2301 AabBab is a relatively young system, estimated to be between 1 and 3 million years old. All four objects show spectroscopic signs of low surface gravity, indicating that they are young and bloated, and still in the process of contracting down. Additionally, Aa and Ab both show weak emissions indicating the ongoing accretion of material. If 1,800 AU is the true separation between Aab and Bab, then both binaries would have completed less than 20 orbits around each other in the last 3 million years. All four objects of this young quadruple system are believed to have formed in the same way stars do.

Figure 2: Comparison of 2M0441+2301 AabBab with theoretical isochrones from two models. From top to bottom, the 5 dotted lines on each chart are the 1 Myr, 5 Myr, 10 Myr, 100 Myr and 1 Gyr isochrones (Myr - million years; Gyr - billion years). Bowler & Hillenbrand (2015).

Bowler & Hillenbrand (2015), "Near-Infrared Spectroscopy of 2M0441+2301 AabBab: A Quadruple System Spanning the Stellar to Planetary Mass Regimes", arXiv:1509.01658 [astro-ph.EP]

Tuesday, September 1, 2015

Red Dwarf Star with a Cold Neptune-Mass Planet

Figure 1: Artist’s impression of a cold Neptune-mass planet.

Combining observations by the Spitzer space telescope and observations by ground-based telescopes, Street et al. (2015) present the discovery of a cold Neptune-mass planet in orbit around a red dwarf star. The planet was detected using a technique known as gravitational microlensing, whereby the gravitational field of a foreground object, in this case, the newfound planet and its host star, acts as a lens, magnifying the light of a more distant background star.

As the planet and its host star crossed the line of sight to the background star, it caused the brightness of the background star to change with time. The change in brightness was observed in the form of a light curve. The gravitational microlensing event is designated as OGLE-2015-BLG-0966, and the planet is identified as OGLE-2015-BLG-0966b, with the lowercase suffix “b” indicating its planetary nature.

By analysing the light curve, the planet is estimated to have 21 ± 2 times the mass of Earth and it orbits a relatively small star with 38 ± 4 percent the Sun’s mass. Both the planet and its host star are estimated to lie 8,000 to 11,000 light years away, in the direction towards the center of the Milky Way galaxy. The projected separation of OGLE-2015-BLG-0966b from its host star is between 2.1 to 2.7 AU, where one AU is the Earth-Sun distance. At such a distance from its host star, OGLE-2015-BLG-0966b receives a relatively low amount of stellar insolation, making it a cold Neptune-mass planet.

Figure 2: Light curve of the gravitational microlensing event OGLE-2015-BLG-0966. Street et al. (2015)

Street et al. (2015), “Spitzer Parallax of OGLE-2015-BLG-0966: A Cold Neptune in the Galactic Disk”, arXiv:1508.07027 [astro-ph.EP]

Saturday, August 29, 2015

A Hot Jupiter with Friends

WASP-47b is a hot-Jupiter in a close-in 4.16 day orbit around a Sun-like star. It has 337 times the mass and 12.7 times the radius of Earth, making it similar in mass and size to Jupiter. Using data from the K2 mission, Becker et al. (2015) present the discovery of two additional planets in the system. The two planets are identified as WASP-47c and WASP-47d. WASP-47c is a super-Earth with an orbital period of 0.79 days, 1.82 times the radius of Earth and is estimated to have less than 8.9 times the mass of Earth. WASP-47d is a Neptune-sized planet with an orbital period of 9.03 days, 3.60 times the Earth’s radius and is estimated to have 8.5 times the Earth’s mass.

With a super-Earth interior to it and a Neptune-sized planet exterior to it, WASP-47d is the first known hot-Jupiter with close-in planetary companions. The orbits of the two planetary companions are coplanar with WASP-47b, and all three planets have almost perfectly circular orbits. WASP-47b and its two close-in companion planets form an extremely compact planetary system. The orbits of all three planets fit well within Mercury’s orbit around the Sun. Nevertheless, calculations indicate that the planetary system is dynamically stable in the long run.

Phase-folded K2 transit light curves of WASP-47b, c and d overlaid with the best-fit transit models (red curves), and binned points (purple circles). Becker et al. (2015)

Hot-Jupiters are basically Jupiter-sized planets that formed further out and subsequently migrated closer in to their host stars. There appears to be a lack of hot-Jupiters with close-in planetary companions. This supports the idea that hot-Jupiters form via the high eccentricity migration (HEM) process. Such a process would destabilise the orbits of other planets in the system, resulting in the lack of close-in planetary companions to hot-Jupiters. However, studies have also shown that not all hot-Jupiters form via the HEM process and these hot-Jupiters can have close-in planetary companions. WASP-47b and its close-in planetary companions demonstrate that Jupiter-sized planets can migrate toward their host stars in a dynamically stable manner.

Becker et al. (2015), “WASP-47: A Hot Jupiter System with Two Additional Planets Discovered by K2”, arXiv:1508.02411 [astro-ph.EP]

Thursday, August 27, 2015

Massive Brown Dwarf in Resonance with its Host Star

CoRoT is a space observatory which hunts for exoplanets by searching for dips in the brightness of stars when a planet happens to pass in front of its host star. Using data collected by CoRoT during its mission, Csizmadia et al. (2015) present the discovery of a massive brown dwarf that orbits a Sun-like star in a close-in orbit with a period of 5.82 days. The brown dwarf is identified as CoRoT-33b. Together with radial velocity measurements, CoRoT-33b is estimated to have 1.1 times the radius and 59 times the mass of Jupiter. The bulk density of CoRoT-33b is 55 g/cm³, several times the density of iron.

Although giant planets and brown dwarfs are similar in size to Jupiter, their masses can range from roughly the same mass as Jupiter up to ~80 times the mass of Jupiter, the maximum mass for brown dwarfs. CoRoT-33b is a relatively rare object and it is in the so called brown dwarf desert. Brown dwarfs in close-in orbits around solar-type stars (i.e. FGK main sequence stars) appear to be ~10 times less common than giant planets in similar close-in orbits around solar-type stars. CoRoT-33b may be in a 2:3 resonance with its host star. The host star of CoRoT-33b rotates twice for ever 3 orbits of CoRoT-33b.

Csizmadia et al. (2015), “Transiting exoplanets from the CoRoT space mission XXVIII. CoRoT-33b, an object in the brown dwarf desert with 2:3 commensurability with its host star”, arXiv:1508.05763 [astro-ph.EP]

Monday, July 27, 2015

A Population of Extremely Long Duration Gamma-Ray Bursts

Gamma-ray bursts (GRBs) are among the most energetic events in the universe. There are three classes of GRBs - short gamma-ray bursts (SGRBs) with durations less than ~2 seconds, long gamma-ray bursts (LGRBs) with durations extending to ~1,000 seconds and ultra-long gamma-ray bursts (ULGRBs) with durations of ~10,000 seconds. SGRBs originate from the mergers of neutron star binaries or neutron star-black hole binaries, while LGRBs are created when the cores of massive stars collapse to form black holes.

ULGRBs have such long burst durations that their progenitors are unlikely to be the same as those for LGRBs. Instead, ULGRBs probably originate from the collapse of giant or supergiant stars into black holes. These stars are orders of magnitude larger than the progenitors of LGRBs, resulting in much longer collapse times. Additionally, these stars have lower densities, resulting in lower mass in-fall rates. The continuous in-fall of material into the nascent black hole drives a GRB with an extremely long duration, leading to an ULGRB. Alternatively, ULGRBs can also be created when white dwarfs get tidally shredded by intermediate mass black holes (IMBH).

Figure 1: Artist’s impression of a gamma-ray burst.

Figure 2: Parameter space for GRBs and other high energy transient phenomena plotted as a function of burst duration versus average luminosity. The classes of events are - soft gamma repeaters (SGRs), short gamma-ray bursts (SGRBs), low-luminosity and long gamma-ray bursts (LLGRBs), long gamma-ray bursts (LGRBs), ultra-long gamma-ray bursts (ULGRBs) and tidal disruption events (TDEs). Andrew Levan (2015).

Recent observations by NASA’s Swift Gamma-Ray Burst Mission have revealed what could be a new population of GRBs with extremely long durations that exceed 100,000 seconds. These extremely long duration GRBs may represent the tidal disruption of main sequence stars by supermassive black holes (SMBHs). When a main sequence star comes too close to a SMBH, the gravitational pull on the star’s outer layers from the SMBH can be stronger than the star’s own gravity. This can cause the star to be completely or partly disrupted.

Material stripped from the star forms an accretion disk around the SMBH and a small fraction of the material may be expelled at relativistic velocities, driving a tidal disruption flare (TDF) that is observed as an extremely long duration GRB. Tidal disruption events (TDEs) involving the tidal shredding of main sequence stars by SMBHs are likely to be the progenitors of extremely long duration GRBs.

Andrew Levan (2015), “Swift discoveries of new populations of extremely long duration high energy transient”, arXiv:1506.03960 [astro-ph.HE] 

Sunday, July 26, 2015

Ultra-Diffuse Galaxies in the Virgo Cluster

Recently, a large number of low surface brightness (LSB) galaxies were discovered in the Coma Cluster - a large cluster of galaxies located over 300 million light years away. Galaxies do not possess well defined boundaries. They simply get fainter and fainter towards their outer regions. As a result, the size of a galaxy is defined by its effective radius, also known as the half-light radius. The effective radius is the radius within which half of the galaxy’s luminosity is emitted.

Many of the LSB galaxies in the Coma Cluster are large, with effective radii between 2 to 5 kpc. One kpc (kiloparsec) is equivalent to 3,260 light years, and for comparison, the effective radius of the Milky Way galaxy is estimated to be ~3.6 kpc. They are also extremely diffuse galaxies with central surface brightnesses between 24 to 26 mag/arcsec². LSB galaxies are vulnerable to tidal perturbations as they move through the cluster and interact with other galaxies. Tidal disruption of a LSB galaxy can strip the galaxy down to only its dense nucleus, leading to the formation of an ultra-compact dwarf (UCD) galaxy.

Mihos et al. (2015) present the discovery of three LSB galaxies in the Virgo Cluster - a much nearer cluster of galaxies located ~50 million light years away. The three LSB galaxies are dubbed VLSB-A, VLSB-B and VLSB-C. They are extremely diffuse galaxies with central surface brightnesses around 27 mag/arcsec² and effective radii between 3 to 10 kpc. All three LSB galaxies appear quite diverse in their physical properties.

VLSB-A appears as a nucleated LSB galaxy with a tidal stream extending off it. This indicates that VLSB-A is presently experiencing tidal perturbations and its diffuse component is currently being stripped away. Since the nucleus of VLSB-A shares the same structural properties as UCD galaxies, VLSB-A will most likely become a new UCD galaxy after its diffuse component is stripped away.

The properties of VLSB-B and VLSB-C are not as clear compared to VLSB-A. However, both VLSB-B and VLSB-C do show a lack of obvious tidal distortion. This suggests they may lie in the outskirts of the Virgo Cluster or may be “falling” into the Virgo Cluster for the first time. Alternatively, they may be highly dominated by dark matter, making them less susceptible to tidal stripping. Interestingly, VLSB-B is appears to host a small population of globular clusters. These globular clusters may indicate the presence of a massive halo of dark matter around the galaxy which means that the galaxy has stronger self-gravity and is therefore more protected against tidal stripping.

Surface brightness of the three LSB galaxies in the Virgo Cluster. Mihos et al. (2015).

Structural properties of the three LSB galaxies in the Virgo Cluster compared with other stellar systems, including early type galaxies in the Virgo Cluster and Fornax Cluster, and in the Local Group, as well as globular clusters and UCD galaxies in the Virgo Cluster, and the LSB galaxies found in the Coma Cluster. The dashed orange lines show the globular cluster selection box, while lines of constant surface brightness are shown in green. Mihos et al. (2015).

Mihos et al. (2015), “Galaxies at the extremes: Ultra-diffuse galaxies in the Virgo Cluster”, arXiv:1507.02270 [astro-ph.GA]

Saturday, July 25, 2015

WOH G64 is a Stellar Behemoth with a Thick Disk

Artist’s impression of WOH G64. Credit: ESO.

WOH G64 is a remarkable red supergiant (RSG) star located 163,000 light years away in the Large Magellanic Cloud (LMC), a satellite galaxy of the Milky Way. The “WHO” in the star’s name comes from the initials of its discoverers - Westerlund, Olander and Hedin; and “G64” indicates that it is the 64th entry in the catalogue published in 1981. The physical properties of WOH G64 are extreme. The star has a relatively cool surface temperature of 3,400 K, but it shines roughly 300,000 times more brightly than does the Sun. With that, WOH G64 is estimated to be 1,540 times larger in size than the Sun, making it one of the largest known RSG stars. If placed at the position of the Sun in the Solar System, the surface of WOH G64 would extend almost to the orbit of Saturn.

Observations of WHO G64 made with the Very Large Telescope Interferometer (VLTI) operated by the European Southern Observatory (ESO) in Chile revealed the presence of an enormous and thick disk of gas and dust around the star. The inner edge of the disk is at ~15 stellar radii from WOH G64, about 120 times the distance of Earth from the Sun. The rest of the disk extends far out from WHO G64, reaching almost one light year in total size. Between 3 to 9 solar masses worth of material is estimated to be in the disk of gas and dust. WHO G64 is at an advance stage of its evolution and is experiencing violent, unstable mass loss. WHO G64 started out with ~25 times the Sun’s mass, but it has since lost between one tenth and a third of its original mass. This stellar behemoth is nearing its final fate as a supernova.

- Levesque et al. (2009), “The Physical Properties of the Red Supergiant WOH G64: The Largest Star Known?”, arXiv:0903.2260 [astro-ph.SR]
- Ohnaka et al. (2009), “Spatially resolved dusty torus toward the red supergiant WOH G64 in the Large Magellanic Cloud”, arXiv:0803.3823 [astro-ph]
- Westerlund, Olander & Hedin (1981), “Supergiant and giant M type stars in the Large Magellanic Cloud”, Astronomy & Astrophysics Supplement Series 43: 267-295

Friday, July 24, 2015

Properties of a Newly Discovered Super-Neptune

Bakos et al. (2015) present the discovery of HATS-7b, a transiting Super-Neptune with an orbital period of 3.185 days around a K dwarf star. The host star of HATS-7b has an effective temperature of 4,990 K, 85 percent the Sun’s mass, 82 percent the Sun’s diameter and shines with 37 percent the luminosity of the Sun. Being a K dwarf star, it is somewhat cooler and less luminous than the Sun - a G dwarf star. The detection of HATS-7b was made using the HATSouth network, comprised of a number of fully automated telescopes in the Southern Hemisphere. The primary goal of the HATSouth network is to search for transiting exoplanets.

Figure 1: Artist’s impression of a Neptune-like planet.

By measuring how much HATS-7b dims its host star when it transits in front, the planet is estimated to be 0.563 times the size of Jupiter. As HATS-7b circles its host star, it also gravitationally perturbs its host star, causing its host star to wobble back and forth. The magnitude of wobbling depends on the planet’s mass. Radial velocity measurements of the host star’s wobbling motion indicate that HATS-7b has 0.120 times the mass of Jupiter, placing it in the mass regime of super-Neptunes. For comparison, the planet Neptune has 0.054 times the mass of Jupiter, or 17.147 times the mass of Earth.

Figure 2: Transit light curve of HATS-7b phase folded to the planet’s orbital period of 3.185 days. The lower panel zooms in on the transit. Bakos et al. (2015).

Figure 3: Radial velocity measurements for the host star of HATS-7b. The gravitational perturbation from HATS-7b induces radial velocity semi-amplitude of 18.4 ± 1.9 m/s on its host star. Bakos et al. (2015).

Knowing the size and mass of HATS-7b allows the planet’s bulk composition to be constrained. Interior models of HATS-7b indicate a hydrogen-helium (H2-He) mass fraction of 18 ± 4 percent if the planet has a rock-iron core and a H2-He envelope, or a H2-He mass fraction of 9 ± 4 percent if the planet has an ice core and a H2-He envelope. If HATS-7b has a rock-iron core and a hydrogen-helium envelope, the best fit models give a core mass of 31 ± 4 Earth-masses and an envelope mass of 7 ± 1.5 Earth-masses. If instead HATS-7b has a ice core and a hydrogen-helium envelope, the best fit models give a core mass of 34.5 ± 4 Earth-masses and an envelope mass of 3.5 ± 1.5 Earth-masses.

The composition of HATS-7b is broadly similar to that of Uranus and Neptune, but quite different from Jupiter and Saturn, which are both predominantly comprised of hydrogen and helium. Super-Neptunes like HATS-7b and the recently discovered HATS-8b (also by the HATSouth network) are important for understanding the transition from ice giants (i.e. Uranus and Neptune) to gas giants (i.e. Jupiter and Saturn). HATS-7b circles in a close-in orbit around its host star at a distance of only 6 million km. This is 25 times closer than Earth is from the Sun. The dayside of HATS-7b is heated to a temperature of over 1,000 K.

Figure 4: Mass-radius diagram of super-Neptunes (planets with less than 0.18 times Jupiter’s mass) and super-Earths with accurately measured masses and radii (less than 20 percent uncertainties). Colour indicates equilibrium temperature. HATS-7b is marked with a box and Neptune is marked with a blue triangle. Abbreviations are: K: Kepler, H: HAT, HS: HATSouth, C: Corot. Bakos et al. (2015).

- Bakos et al. (2015), “HATS-7b: A Hot Super Neptune Transiting a Quiet K Dwarf Star”, arXiv:1507.01024 [astro-ph.EP]
- Bayliss et al. (2015), “HATS-8b: A Low-Density Transiting Super-Neptune”, arXiv:1506.01334 [astro-ph.EP]