HD 106906: a Case Study for External Perturbations of a Debris Disk

Total Page:16

File Type:pdf, Size:1020Kb

HD 106906: a Case Study for External Perturbations of a Debris Disk The Astrophysical Journal Letters, 837:L6 (7pp), 2017 March 1 https://doi.org/10.3847/2041-8213/aa61a7 © 2017. The American Astronomical Society. All rights reserved. HD 106906: A Case Study for External Perturbations of a Debris Disk Erika R. Nesvold1, Smadar Naoz2,3, and Michael P. Fitzgerald2 1 Department of Terrestrial Magnetism, Carnegie Institution for Science, 5241 Broad Branch Road, Washington, DC 20015, USA 2 Department of Physics and Astronomy, UCLA, 475 Portola Plaza, Los Angeles, CA 90095, USA 3 Mani L. Bhaumik Institute for Theoretical Physics, Department of Physics and Astronomy, UCLA, Los Angeles, CA 90095, USA Received 2017 February 10; revised 2017 February 17; accepted 2017 February 17; published 2017 March 1 Abstract Models of debris disk morphology are often focused on the effects of a planet orbiting interior to or within the disk. Nonetheless, an exterior planetary-mass perturber can also excite eccentricities in a debris disk, via Laplace– Lagrange secular perturbations in the coplanar case or Kozai–Lidov perturbations for mutually inclined companions and disks. HD 106906 is an ideal example of such a a system, as it harbors a confirmed exterior 11 MJup companion at a projected separation of 650 au outside a resolved, asymmetric disk. We use collisional and dynamical simulations to investigate the interactions between the disk and the companion, and to use the disk’s observed morphology to place constraints on the companion’s orbit. We conclude that the disk’s observed morphology is consistent with perturbations from the observed exterior companion. Generalizing this result, we suggest that exterior perturbers, as well as interior planets, should be considered when investigating the cause of observed asymmetries in a debris disk. Key words: celestial mechanics – circumstellar matter – methods: numerical – planetary systems – planet–disk interactions – stars: individual (HD 106906) 1. Introduction grains (Kalas et al. 2015; Lagrange et al. 2016). These Circumstellar debris disks are produced by the rocky and icy observations noted four major features of the disk morphology material leftover from the formation of the star and any planets and system geometry: in the system. To date, over 1700 debris disks have been 1. The position angle (PA) of the disk is oriented ~21 detected via the excess infrared emission in their star’s spectral counterclockwise from the PA of the companion, which energy distribution (Cotten & Song 2016), and over 40 have constrains the orbit of the companion relative to the disk. been resolved with optical or infrared imaging (http:// 2. The inner disk has little to no vertical extension. While ) circumstellardisks.org . The architecture of the underlying Kalas et al. (2015) tentatively suggested the presence of a planetary system can leave a distinct imprint on the morph- “warp” in the disk’s vertical structure on the west side of ( ology of a debris disk Mouillet et al. 1997; Wyatt et al. 1999; the disk, this warp was not confirmed by Lagrange et al. Matthews et al. 2014; Nesvold & Kuchner 2015b; Lee & (2016). This lack of vertical extension indicates that the Chiang 2016; Nesvold et al. 2016). inclinations of the disk particles have not been excited. Modeling debris disk morphology is often focused on the 3. The east side of the disk is brighter than the west side in effects of a planetary-mass perturber orbiting interior to or GPI and SPHERE near-infrared images. within the disk (Mouillet et al. 1997; Chiang et al. 2009; 4. Kalas et al. (2015) observed a faint extension on the west Nesvold & Kuchner 2015a; Pearce & Wyatt 2015). None- theless, exterior companions have been detected and inferred side of the disk out to nearly 500 au, but only diffuse for several systems (Rodriguez & Zuckerman 2012; Bailey emission on the east side. et al. 2014; Mawet et al. 2015), and dynamical modeling These latter two features indicate that the disk may be an suggests that an exterior perturber can also excite eccentricities eccentric ring, which will exhibit a brightness asymmetry – of the particles in a debris disk, via Laplace Lagrange secular toward the pericenter side (“pericenter glow”; Wyatt ( ) perturbations in the near-coplanar case Thébault et al. 2012 or et al. 1999) and a faint, extended tail toward the apocenter Kozai–Lidov perturbations for mutually inclined companions ( ) ( ) side Lee & Chiang 2016 . and disks Nesvold et al. 2016 , inducing asymmetries in the We modeled the HD 106906 system to demonstrate that the disk and triggering a collisional cascade. Collisions between observed exterior companion can shape the disk into a flat, the disk particles produce smaller dust grains whose thermal eccentric ring, and that all four of these morphological features emission or scattered light can then be spatially resolved with can be reproduced without invoking the presence of a second infrared or optical imaging (Wyatt 2008). HD 106906 is an ideal example of a system with an exterior companion. We also used the observed features and asymme- perturber, as it harbors a confirmed exterior companion with a tries of the HD 106906 disk to place constraints on the orbit of the observed companion. In Section 2, we describe the model-atmosphere-derived mass of 11 MJup at a projected separation of 650 au outside a resolved disk (Bailey collisional and dynamical simulations we performed on the et al. 2014). Scattered-light imaging of the disk with the parent bodies and dust grains in the HD 106906 disk. In Gemini Planet Imager (GPI), the Hubble Space Telescope’s Section 3, we present the simulated brightness images Advanced Camera for Surveys (HST/ACS), and SPHERE has produced by our simulations for comparison with observations. revealed that the disk is a ring viewed nearly edge-on In 4, we discuss the implication of these results and show how (inclination ~85), with a inner region cleared of small dust they can be used to constrain the orbit of HD 106906b. In 1 The Astrophysical Journal Letters, 837:L6 (7pp), 2017 March 1 Nesvold, Naoz, & Fitzgerald Table 1 such that the simulated companion’s orbit could reproduce the Initial Conditions of the Disk and Companion for the Simulation position of the observed companion. Parameter Initial Disk Values HD 106906b 2.2. SMACK versus Collisionless N-body Semimajor Axis (au) 65–85 700 Eccentricity 0–0.01 0.7 To measure the effects of collisions on the dynamics of the Inclination (°) 0–0.29 8.5 disk particles, we also performed a collisionless N-body Longitude of Nodes (°) 0–360 90 simulation of the disk using the Wisdom–Holman integrator Argument of Pericenter (°) 0–360 −90 of REBOUND with collision detection and resolution turned Optical Depth 1.4´ 10-3 L off. The collisionless N-body simulation used the same ( −3) L Density gcm 1.0 companion and disk parameters as the SMACK simulation (Table 1), with 10,000 test particles to represent the disk. Figure 1 shows the time evolution of the simulated disk’s Section 5, we summarize our conclusions and suggest average eccentricity, inclination, longitude of nodes, and opportunities for future work. argument of pericenter. Although there are small variations, most notably in the average eccentricity, between the SMACK 2. Simulations simulation and the collisionless N-body simulation, the maximum difference for each parameter is 10%, indicating Given that collisions between particles in a disk with that fragmenting collisions have a minimal effect on the fi ( -3 suf ciently high optical depth LIR L* »´1.4 10 for HD dynamics of this system. 106906 Chen et al. 2011) will both produce the small grains seen in observations and may affect the dynamics of the disk, 2.3. Dust Model we simulated the HD 106906 system using the Superparticle- Method Algorithm for Collisions in Kuiper belts and debris To generate the simulated images of the dust grains in the disks (SMACK; Nesvold et al. 2013). We then recorded the HD 106906 system, we adapted the method of Lee & Chiang dust-producing encounters between parent bodies, simulated (2016), which extended the dust orbit calculations of Wyatt the orbits of the generated dust grains under the influence of et al. (1999) to include estimates of the surface brightness. Our radiative forces following the method of Lee & Chiang (2016), SMACK simulation output the locations of dust-producing then simulated the surface brightness of the dust using a collisions during the 15 Myr simulation, as well as the orbits of Henyey–Greenstein scattering phase function (Henyey & the parent bodies producing the dust. We selected the first 104 Greenstein 1941). dust production events occurring after time t=5 Myr. For each dust production event, we generated 10 dust orbits, each with a β value randomly chosen from a power-law distribution 2.1. SMACK Model with an index 3/2 (where b » FFrad grav represents the ratio of SMACK is based on the N-body integrator REBOUND the radiative and gravitational forces acting on a dust grain). (Rein & Liu 2012), but approximates each particle in the The maximum possible value for the β value was set by the integrator as a collection of bodies with a range of sizes parent body’s orbit: between 1 mm and 10 cm in diameter, traveling on the same “ ” 1 - ep orbit. This group of bodies is called a superparticle and is bmax = ,1() characterized by a size distribution, position, and velocity. The 21()+ efp cosp superparticles act as test particles in the integration, and orbit where e and f are the parent body’s eccentricity and true the star under the influence of perturbations by any planets in p p the simulation. Each superparticle is approximated as a sphere anomaly, respectively. The semimajor axis a, eccentricity e, with some finite radius.
Recommended publications
  • Debris Dust Around Main Sequence Stars
    Debris Dust Around Main Sequence Stars et al. (2013) Kalas Chris5ne H. Chen STScI, September 2016 1 Exoplanetary Systems Exoplanet Observaons Debris Disk Observaons 2 Outline • The HR 4796 System • Training Students Using the KecK LWS • Spitzer GTO Programs – A Search for Terrestrial Planetary Debris Systems and Other Planetary Debris DisKs – Spectroscopy of Protostellar, Protoplanetary and Debris DisKs – Dust Around Main Sequence A-type Stars – The Fabulous Four Debris DisKs 3 Early Debris DisK WorK Timeline • 1983 IRAS launches • 1984 Smith & Terrile spaally resolve the β Pic disK in scaered light using a coronagraph • 1986 Gille] accurately measures “infrared excess” toward Vega, Fomalhaut and β Pic from pointed IRAS observaons • 1991 Jura discovers HR 4796 IRAS infrared excess • 1991 Telesco and KnacKe discover spectroscopic evidence for silicates around β Pic • 1993 BacKman review ar5cle “Main Sequence Stars with Circumstellar Solid Material: The Vega Phenomenon” is published in Protostars and Planets III • 1998 Koerner and Jayawardhana resolve the HR 4796A disK in thermal emission using KecK/MIRLIN and Blanco/OSCIR • 2003 Spitzer launches • 2014 Gemini Planet Imager commissioning HR 4796A Infrared Excess Discovery HR 4796B Secondary Star Discovery • First es5mate for the grain temperature based on simple blacK body modeling, Tgr = 110 K with a predic5on for the distance of the grains from the star, ~40 AU • First grain size constrain (> 10 μm) based on the upper limit for the size of the system (<5” at 20 μm) • First calculaon of the Poyn5ng-Robertson drag life5me for this disK demonstrang that it must be a debris disK HR 4796A Planetary Companion Constraints • Central clearing may be created by a planetary mass object • SpecKle observaons constrain the mass to be < 0.125 M¤ The HR 4796A DisK Resolved! (Leo) HST NICMOS F1600W and F1100W coronagraphic images showing discovery of the light scaered from the dust (Schneider et al.
    [Show full text]
  • Exoplanet.Eu Catalog Page 1 # Name Mass Star Name
    exoplanet.eu_catalog # name mass star_name star_distance star_mass OGLE-2016-BLG-1469L b 13.6 OGLE-2016-BLG-1469L 4500.0 0.048 11 Com b 19.4 11 Com 110.6 2.7 11 Oph b 21 11 Oph 145.0 0.0162 11 UMi b 10.5 11 UMi 119.5 1.8 14 And b 5.33 14 And 76.4 2.2 14 Her b 4.64 14 Her 18.1 0.9 16 Cyg B b 1.68 16 Cyg B 21.4 1.01 18 Del b 10.3 18 Del 73.1 2.3 1RXS 1609 b 14 1RXS1609 145.0 0.73 1SWASP J1407 b 20 1SWASP J1407 133.0 0.9 24 Sex b 1.99 24 Sex 74.8 1.54 24 Sex c 0.86 24 Sex 74.8 1.54 2M 0103-55 (AB) b 13 2M 0103-55 (AB) 47.2 0.4 2M 0122-24 b 20 2M 0122-24 36.0 0.4 2M 0219-39 b 13.9 2M 0219-39 39.4 0.11 2M 0441+23 b 7.5 2M 0441+23 140.0 0.02 2M 0746+20 b 30 2M 0746+20 12.2 0.12 2M 1207-39 24 2M 1207-39 52.4 0.025 2M 1207-39 b 4 2M 1207-39 52.4 0.025 2M 1938+46 b 1.9 2M 1938+46 0.6 2M 2140+16 b 20 2M 2140+16 25.0 0.08 2M 2206-20 b 30 2M 2206-20 26.7 0.13 2M 2236+4751 b 12.5 2M 2236+4751 63.0 0.6 2M J2126-81 b 13.3 TYC 9486-927-1 24.8 0.4 2MASS J11193254 AB 3.7 2MASS J11193254 AB 2MASS J1450-7841 A 40 2MASS J1450-7841 A 75.0 0.04 2MASS J1450-7841 B 40 2MASS J1450-7841 B 75.0 0.04 2MASS J2250+2325 b 30 2MASS J2250+2325 41.5 30 Ari B b 9.88 30 Ari B 39.4 1.22 38 Vir b 4.51 38 Vir 1.18 4 Uma b 7.1 4 Uma 78.5 1.234 42 Dra b 3.88 42 Dra 97.3 0.98 47 Uma b 2.53 47 Uma 14.0 1.03 47 Uma c 0.54 47 Uma 14.0 1.03 47 Uma d 1.64 47 Uma 14.0 1.03 51 Eri b 9.1 51 Eri 29.4 1.75 51 Peg b 0.47 51 Peg 14.7 1.11 55 Cnc b 0.84 55 Cnc 12.3 0.905 55 Cnc c 0.1784 55 Cnc 12.3 0.905 55 Cnc d 3.86 55 Cnc 12.3 0.905 55 Cnc e 0.02547 55 Cnc 12.3 0.905 55 Cnc f 0.1479 55
    [Show full text]
  • High-Precision HST/WFC3/IR Time-Resolved Observations of Directly Imaged Exoplanet HD 106906B
    The Astronomical Journal, 159:140 (13pp), 2020 April https://doi.org/10.3847/1538-3881/ab6f65 © 2020. The American Astronomical Society. All rights reserved. Cloud Atlas: High-precision HST/WFC3/IR Time-resolved Observations of Directly Imaged Exoplanet HD 106906b Yifan Zhou1,2,15 , Dániel Apai1,3,4 , Luigi R. Bedin5, Ben W. P. Lew3 , Glenn Schneider1 , Adam J. Burgasser6 , Elena Manjavacas7 , Theodora Karalidi8 , Stanimir Metchev9,10 , Paulo A. Miles-Páez11,16 , Nicolas B. Cowan12 , Patrick J. Lowrance13 , and Jacqueline Radigan14 1 Department of Astronomy/Steward Observatory, The University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA; [email protected] 2 Department of Astronomy/McDonald Observatory, The University of Texas, 2515 Speedway, Austin, TX 78712, USA 3 Department of Planetary Science/Lunar and Planetary Laboratory, The University of Arizona, 1640 E. University Boulevard, Tucson, AZ 85718, USA 4 Earths in Other Solar Systems Team, NASA Nexus for Exoplanet System Science, USA 5 INAF—Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I-35122 Padova, Italy 6 Center for Astrophysics and Space Science, University of California San Diego, La Jolla, CA 92093, USA 7 W.M. Keck Observatory, 65-1120 Mamalahoa Hwy. Kamuela, HI 96743, USA 8 Department of Physics, University of Central Florida, 4111 Libra Drive, Orlando, FL 32816, USA 9 Department of Physics & Astronomy and Centre for Planetary Science and Exploration, The University of Western Ontario, London, Ontario N6A 3K7, Canada 10 Department of Astrophysics,
    [Show full text]
  • Exoplanet.Eu Catalog Page 1 Star Distance Star Name Star Mass
    exoplanet.eu_catalog star_distance star_name star_mass Planet name mass 1.3 Proxima Centauri 0.120 Proxima Cen b 0.004 1.3 alpha Cen B 0.934 alf Cen B b 0.004 2.3 WISE 0855-0714 WISE 0855-0714 6.000 2.6 Lalande 21185 0.460 Lalande 21185 b 0.012 3.2 eps Eridani 0.830 eps Eridani b 3.090 3.4 Ross 128 0.168 Ross 128 b 0.004 3.6 GJ 15 A 0.375 GJ 15 A b 0.017 3.6 YZ Cet 0.130 YZ Cet d 0.004 3.6 YZ Cet 0.130 YZ Cet c 0.003 3.6 YZ Cet 0.130 YZ Cet b 0.002 3.6 eps Ind A 0.762 eps Ind A b 2.710 3.7 tau Cet 0.783 tau Cet e 0.012 3.7 tau Cet 0.783 tau Cet f 0.012 3.7 tau Cet 0.783 tau Cet h 0.006 3.7 tau Cet 0.783 tau Cet g 0.006 3.8 GJ 273 0.290 GJ 273 b 0.009 3.8 GJ 273 0.290 GJ 273 c 0.004 3.9 Kapteyn's 0.281 Kapteyn's c 0.022 3.9 Kapteyn's 0.281 Kapteyn's b 0.015 4.3 Wolf 1061 0.250 Wolf 1061 d 0.024 4.3 Wolf 1061 0.250 Wolf 1061 c 0.011 4.3 Wolf 1061 0.250 Wolf 1061 b 0.006 4.5 GJ 687 0.413 GJ 687 b 0.058 4.5 GJ 674 0.350 GJ 674 b 0.040 4.7 GJ 876 0.334 GJ 876 b 1.938 4.7 GJ 876 0.334 GJ 876 c 0.856 4.7 GJ 876 0.334 GJ 876 e 0.045 4.7 GJ 876 0.334 GJ 876 d 0.022 4.9 GJ 832 0.450 GJ 832 b 0.689 4.9 GJ 832 0.450 GJ 832 c 0.016 5.9 GJ 570 ABC 0.802 GJ 570 D 42.500 6.0 SIMP0136+0933 SIMP0136+0933 12.700 6.1 HD 20794 0.813 HD 20794 e 0.015 6.1 HD 20794 0.813 HD 20794 d 0.011 6.1 HD 20794 0.813 HD 20794 b 0.009 6.2 GJ 581 0.310 GJ 581 b 0.050 6.2 GJ 581 0.310 GJ 581 c 0.017 6.2 GJ 581 0.310 GJ 581 e 0.006 6.5 GJ 625 0.300 GJ 625 b 0.010 6.6 HD 219134 HD 219134 h 0.280 6.6 HD 219134 HD 219134 e 0.200 6.6 HD 219134 HD 219134 d 0.067 6.6 HD 219134 HD
    [Show full text]
  • Exoplanetary Atmospheres
    Exoplanetary Atmospheres Nikku Madhusudhan1,2, Heather Knutson3, Jonathan J. Fortney4, Travis Barman5,6 The study of exoplanetary atmospheres is one of the most exciting and dynamic frontiers in astronomy. Over the past two decades ongoing surveys have revealed an astonishing diversity in the planetary masses, radii, temperatures, orbital parameters, and host stellar properties of exo- planetary systems. We are now moving into an era where we can begin to address fundamental questions concerning the diversity of exoplanetary compositions, atmospheric and interior processes, and formation histories, just as have been pursued for solar system planets over the past century. Exoplanetary atmospheres provide a direct means to address these questions via their observable spectral signatures. In the last decade, and particularly in the last five years, tremendous progress has been made in detecting atmospheric signatures of exoplanets through photometric and spectroscopic methods using a variety of space-borne and/or ground-based observational facilities. These observations are beginning to provide important constraints on a wide gamut of atmospheric properties, including pressure-temperature profiles, chemical compositions, energy circulation, presence of clouds, and non-equilibrium processes. The latest studies are also beginning to connect the inferred chemical compositions to exoplanetary formation conditions. In the present chapter, we review the most recent developments in the area of exoplanetary atmospheres. Our review covers advances in both observations and theory of exoplanetary atmospheres, and spans a broad range of exoplanet types (gas giants, ice giants, and super-Earths) and detection methods (transiting planets, direct imaging, and radial velocity). A number of upcoming planet-finding surveys will focus on detecting exoplanets orbiting nearby bright stars, which are the best targets for detailed atmospheric characterization.
    [Show full text]
  • Arxiv:2108.13437V1 [Astro-Ph.EP] 30 Aug 2021 Perienced Giant Impacts, Tidal Friction, and Gravitational Forcing (E.G
    Draft version September 1, 2021 Typeset using LATEX twocolumn style in AASTeX631 Obliquity Constraints on the Planetary-mass Companion HD 106906 b Marta L. Bryan,1 Eugene Chiang,1 Caroline V. Morley,2 Gregory N. Mace,2 and Brendan P. Bowler2 1Department of Astronomy 501 Campbell Hall University of California Berkeley Berkeley, CA 94720-3411, USA 2Department of Astronomy The University of Texas at Austin Austin, TX 78712, USA ABSTRACT We constrain the angular momentum architecture of HD 106906, a 13 ± 2 Myr old system in the ScoCen complex composed of a compact central binary, a widely separated planetary-mass tertiary HD 106906 b, and a debris disk nested between the binary and tertiary orbital planes. We measure the orientations of three vectors: the companion spin axis, companion orbit normal, and disk normal. Using near-IR high-resolution spectra from Gemini/IGRINS, we obtain a projected rotational velocity of v sin ip = 9.5 ± 0.2 km/s for HD 106906 b. This measurement together with a published photometric rotation period implies the companion is viewed nearly pole-on, with a line-of-sight spin axis inclination ◦ ◦ of ip = 14 ± 4 or 166 ± 4 . By contrast, the debris disk is known to be viewed nearly edge-on. The likely misalignment of all three vectors suggests HD 106906 b formed by gravitational instability in a turbulent environment, either in a disk or cloud setting. Keywords: Exoplanet systems { Exoplanet formation { Exoplanet evolution { High resolution spec- troscopy { Astrostatistics 1. INTRODUCTION These processes and others can apply to exoplanets. Planetary obliquity measurements inform our under- Theoretical work shows that obliquities can be excited standing of how planets form and evolve.
    [Show full text]
  • Astrotalk: Behind the News Headlines of May 2017
    AstroTalk: Behind the news headlines of May 2017 Richard de Grijs (何锐思) (Kavli Institute for Astronomy and Astrophysics, Peking University) Planetary formation is disks of dust and gas unveiled Newborn stars are typically located in disks of gas and dust. When planets first begin to form, rings of rocky and icy material (‘planetesimals’) form. The dust in those rings starts to stick together, growing until clumps develop that are large enough to attract other clumps because of their gravity. Astronomers believe that the process of forming planets and dissipating the disk takes about 10 million years. Many mysteries remain, however, including the tendency of dust not to stick together, and the likelihood that colliding clumps could break apart rather than agglomerate. As analogues to our own Solar System’s ‘Kuiper Belt’ or ‘Oort Cloud,’ the disks of debris left over from planet formation can be detected by astronomers and studied to help understand the processes that create planetary systems. Astronomers recently presented new observations of a nearby planetary system known as ‘61 Virginis’ (‘61 Vir’) and its debris disk. 61 Vir is a 4.6-billion-year- old star, about the size of our Sun, which is located approximately 28 light-years away. At least three planets orbit the parent star, which are five, 18, and 23 times more massive than the Earth. One of the most intriguing features of this system is its debris disk, which extends from 30 to at least 100 astronomical units (‘au,’ the average distance from the Sun to the Earth) from the star. A team of astronomers led by Sebastian Marino of the University of Cambridge (UK) has performed observations of 61 Vir’s debris disk using the Atacama Large Millimetre/submillimetre Array (ALMA) in Chile.
    [Show full text]
  • Direct Imaging Discovery of a Second Planet Candidate Around the Possibly Transiting Planet Host CVSO 30 ⋆
    Astronomy & Astrophysics manuscript no. CVSO c ESO 2016 March 17, 2016 Direct Imaging discovery of a second planet candidate around the possibly transiting planet host CVSO 30 ⋆ T. O. B. Schmidt1, 2, R. Neuhäuser2, C. Briceño3, N. Vogt4, St. Raetz5, A. Seifahrt6, C. Ginski7, M. Mugrauer2, S. Buder2, 8, C. Adam2, P. Hauschildt1, S. Witte1, Ch. Helling9, and J. H. M. M. Schmitt1 1 Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany, e-mail: [email protected] 2 Astrophysikalisches Institut und Universitäts-Sternwarte, Universität Jena, Schillergäßchen 2-3, 07745 Jena, Germany 3 Cerro Tololo Inter-American Observatory CTIO/AURA/NOAO, Colina El Pino s/n. Casilla 603, 1700000 La Serena, Chile 4 Instituto de Física y Astronomía, Universidad de Valparaíso, Avenida Gran Bretaña 1111, 2340000 Valparaíso, Chile 5 European Space Agency ESA, ESTEC, SRE-S, Keplerlaan 1, NL-2201 AZ Noordwijk, the Netherlands 6 Department of Astronomy and Astrophysics, University of Chicago, 5640 S. Ellis Ave., Chicago, IL 60637, USA 7 Sterrewacht Leiden, PO Box 9513, Niels Bohrweg 2, NL-2300RA Leiden, the Netherlands 8 Max-Planck-Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany 9 School of Physics and Astronomy SUPA, University of St. Andrews, North Haugh, St. Andrews, KY16 9SS, UK Received 2015; accepted ABSTRACT Context. Direct Imaging has developed into a very successful technique for the detection of exoplanets in wide orbits, especially around young stars. Directly imaged planets can both be followed astrometrically on their orbits and observed spectroscopically, and thus provide an essential tool for our understanding of the early Solar System. Aims. We surveyed the 25 Ori association for Direct Imaging companions, having an age of only few million years.
    [Show full text]
  • Arxiv:1312.1265V1 [Astro-Ph.EP] 4 Dec 2013
    Accepted to ApJL Preprint typeset using LATEX style emulateapj v. 5/2/11 HD 106906 b: A PLANETARY-MASS COMPANION OUTSIDE A MASSIVE DEBRIS DISK Vanessa Bailey1, Tiffany Meshkat2, Megan Reiter1, Katie Morzinski1*, Jared Males1*, Kate Y. L. Su1, Philip M. Hinz1, Matthew Kenworthy2, Daniel Stark1, Eric Mamajek3, Runa Briguglio4, Laird M. Close1, Katherine B. Follette1, Alfio Puglisi4, Timothy Rodigas1,5, Alycia J. Weinberger5, and Marco Xompero4 1 Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA; [email protected] 2 Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden, The Netherlands 3 Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627-0171, USA 4 Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, I-50125 Firenze, Italy and 5 Carnegie Institution of Washington, Department of Terrestrial Magnetism, 5241 Broad Branch Road NW, Washington, DC 20015, USA Accepted to ApJL ABSTRACT We report the discovery of a planetary-mass companion, HD 106906 b, with the new Magellan Adaptive Optics (MagAO) + Clio2 system. The companion is detected with Clio2 in three bands: J, 0 00 KS, and L , and lies at a projected separation of 7: 1 (650 AU). It is confirmed to be comoving with its 13±2 Myr-old F5 host using Hubble Space Telescope/Advanced Camera for Surveys astrometry over a time baseline of 8.3 yr. DUSTY and COND evolutionary models predict the companion's luminosity corresponds to a mass of 11 ± 2 MJup, making it one of the most widely separated planetary-mass companions known. We classify its Magellan/Folded-Port InfraRed Echellette J=H=K spectrum as L2:5 ± 1; the triangular H-band morphology suggests an intermediate surface gravity.
    [Show full text]
  • Effects of Rotation Arund the Axis on the Stars, Galaxy and Rotation of Universe* Weitter Duckss1
    Effects of Rotation Arund the Axis on the Stars, Galaxy and Rotation of Universe* Weitter Duckss1 1Independent Researcher, Zadar, Croatia *Project: https://www.svemir-ipaksevrti.com/Universe-and-rotation.html; (https://www.svemir-ipaksevrti.com/) Abstract: The article analyzes the blueshift of the objects, through realized measurements of galaxies, mergers and collisions of galaxies and clusters of galaxies and measurements of different galactic speeds, where the closer galaxies move faster than the significantly more distant ones. The clusters of galaxies are analyzed through their non-zero value rotations and gravitational connection of objects inside a cluster, supercluster or a group of galaxies. The constant growth of objects and systems is visible through the constant influx of space material to Earth and other objects inside our system, through percussive craters, scattered around the system, collisions and mergers of objects, galaxies and clusters of galaxies. Atom and its formation, joining into pairs, growth and disintegration are analyzed through atoms of the same values of structure, different aggregate states and contiguous atoms of different aggregate states. The disintegration of complex atoms is followed with the temperature increase above the boiling point of atoms and compounds. The effects of rotation around an axis are analyzed from the small objects through stars, galaxies, superclusters and to the rotation of Universe. The objects' speeds of rotation and their effects are analyzed through the formation and appearance of a system (the formation of orbits, the asteroid belt, gas disk, the appearance of galaxies), its influence on temperature, surface gravity, the force of a magnetic field, the size of a radius.
    [Show full text]
  • Arxiv:2108.13437V1 [Astro-Ph.EP] 30 Aug 2021 Perienced Giant Impacts, Tidal Friction, and Gravitational Forcing (E.G
    Draft version September 1, 2021 Typeset using LATEX twocolumn style in AASTeX631 Obliquity Constraints on the Planetary-mass Companion HD 106906 b Marta L. Bryan,1 Eugene Chiang,1 Caroline V. Morley,2 Gregory N. Mace,2 and Brendan P. Bowler2 1Department of Astronomy 501 Campbell Hall University of California Berkeley Berkeley, CA 94720-3411, USA 2Department of Astronomy The University of Texas at Austin Austin, TX 78712, USA ABSTRACT We constrain the angular momentum architecture of HD 106906, a 13 ± 2 Myr old system in the ScoCen complex composed of a compact central binary, a widely separated planetary-mass tertiary HD 106906 b, and a debris disk nested between the binary and tertiary orbital planes. We measure the orientations of three vectors: the companion spin axis, companion orbit normal, and disk normal. Using near-IR high-resolution spectra from Gemini/IGRINS, we obtain a projected rotational velocity of v sin ip = 9.5 ± 0.2 km/s for HD 106906 b. This measurement together with a published photometric rotation period implies the companion is viewed nearly pole-on, with a line-of-sight spin axis inclination ◦ ◦ of ip = 14 ± 4 or 166 ± 4 . By contrast, the debris disk is known to be viewed nearly edge-on. The likely misalignment of all three vectors suggests HD 106906 b formed by gravitational instability in a turbulent environment, either in a disk or cloud setting. Keywords: Exoplanet systems { Exoplanet formation { Exoplanet evolution { High resolution spec- troscopy { Astrostatistics 1. INTRODUCTION These processes and others can apply to exoplanets. Planetary obliquity measurements inform our under- Theoretical work shows that obliquities can be excited standing of how planets form and evolve.
    [Show full text]
  • The Late-Time Formation and Dynamical Signatures of Small Planets
    The Late-Time Formation and Dynamical Signatures of Small Planets By Eve Jihyun Lee A dissertation submitted in partial satisfaction of the requirements for the degree of Doctor of Philosophy in Astrophysics in the Graduate Division of the University of California, Berkeley Committee in charge: Professor Eugene Chiang, Chair Professor Eliot Quataert Professor David M. Romps Spring 2017 The Late-Time Formation and Dynamical Signatures of Small Planets Copyright 2017 by Eve Jihyun Lee 1 Abstract The Late-Time Formation and Dynamical Signatures of Small Planets by Eve Jihyun Lee Doctor of Philosophy in Astrophysics University of California, Berkeley Professor Eugene Chiang, Chair The riddle posed by super-Earths is that they are not Jupiters: their core masses are large enough to trigger runaway gas accretion, yet somehow super-Earths accreted atmospheres that weigh only a few percent of their total mass. In this thesis, I demonstrate that this puzzle is solved if super-Earths formed late, in the inner cavities of transitional disks. Super- puffs present the inverse problem of being too voluminous for their small masses. I show that super-puffs most easily acquire their thick atmospheres as dust-free, rapidly cooling worlds outside 1 AU, and then migrate in just after super-Earths appear. Super-Earths and Earth- sized planets around FGKM dwarfs are evenly distributed in log orbital period down to ∼10 days, but dwindle in number at shorter periods. I demonstrate that both the break at ∼10 days and the slope of the occurrence rate down to ∼1 day can be reproduced if planets form in disks that are truncated by their host star magnetospheres at co-rotation.
    [Show full text]