Radio OH observations of 9P/Tempel 1 before and after Deep Impact   总被引：1，自引：0，他引：1  

Ellen S. Howell  Amy J. Lovell  F. Peter Schloerb 《Icarus》2007,187(1):228-239

We observed 18-cm OH emission in Comet 9P/Tempel 1 before and after Deep Impact. Observations using the Arecibo Observatory 305 m telescope took place between 8 April and 9 June, 2005, followed by post-impact observations using the National Radio Astronomy Observatory 100 m Green Bank Telescope 4-12 July, 2005. The resulting spectra were analyzed with a kinematic Monte Carlo model which allows estimation of the OH production rate, neutral gas outflow velocity, and distribution of the out-gassing from the nucleus. We detected typically 24% variability from the overall OH production rate trend in the two months leading up to the impact, and no dramatic increase in OH production in the days post-impact. Generally, the coma is well-described, within uncertainties, by a symmetric model with OH production rates from 1.6 to , and mean water outflow velocity of . At these low production rates, collisional quenching is expected to occur only within 20,000 km of the nucleus. However, our best-fit average quenching radius is 64,200 ± 22,000 km in April and May.  相似文献   

Submillimeter photometry and lightcurves of Ceres and other large asteroids     

Matthew A. Chamberlain  Amy J. Lovell 《Icarus》2009,202(2):487-501

Photometry and thermal lightcurves of six large asteroids (1-Ceres, 2-Pallas, 3-Juno, 12-Victoria, 85-Io and 511-Davida) have been observed at 870 μm (345 GHz) using the MPIfR 19-Channel Bolometer of the Heinrich-Hertz Submillimeter Telescope. Only Ceres displayed a lightcurve with an amplitude (∼50%, peak to peak) that was significantly greater than the uncertainty in the observations. When thermal fluxes and brightness temperatures are corrected for heliocentric distance and albedo, there is a significant relation with the sub-solar latitude of the asteroid, or the local season of the asteroid. No such trend can be found between observations with solar phase angle. These results are evidence that most of the submillimeter thermal radiation is emitted from below the diurnal thermal wave. Comparing the observed trend with model output suggests that the submillimeter radiation from all the asteroids we observed is best modeled by surface material with low thermal inertia (<15 J m⁻² s^−0.5 K⁻¹, consistent with mid-infrared observations of large main-belt asteroids) and a refractive index closer to unity relative to densities inferred from radar experiments, implying a veneer of material over the asteroid surface with a density less than 1000 kg m⁻³. More data with better signal-to-noise and aspect coverage could improve these models and constrain physical properties of asteroid surface materials. This would also allow asteroids to be used as calibration sources with accurately known and stable, broadband fluxes at long wavelengths.  相似文献   

Revisiting the relativistic ejection event in XTE J1550−564 during the 1998 outburst     

D. C. Hannikainen  R. W. Hunstead  K. Wu  V. McIntyre  J. E. J. Lovell  D. Campbell-Wilson  M. L. McCollough  J. Reynolds  A. K. Tzioumis 《Monthly notices of the Royal Astronomical Society》2009,397(1):569-576

We revisit the discovery outburst of the X-ray transient XTE J1550−564 during which relativistic jets were observed in 1998 September, and review the radio images obtained with the Australian Long Baseline Array, and light curves obtained with the Molonglo Observatory Synthesis Telescope and the Australia Telescope Compact Array. Based on H i spectra, we constrain the source distance to between 3.3 and 4.9 kpc. The radio images, taken some 2 d apart, show the evolution of an ejection event. The apparent separation velocity of the two outermost ejecta is at least  1.3 c   and may be as large as  1.9 c   ; when relativistic effects are taken into account, the inferred true velocity is  ≥ 0.8 c   . The flux densities appear to peak simultaneously during the outburst, with a rather flat (although still optically thin) spectral index of −0.2.  相似文献   

Collisional Quenching of OH Radio Emission from Comet Hale-Bopp     

Schloerb  F. P.  Devries  C. H.  Lovell  A. J.  Irvine  W. M.  Senay  M.  Wootten  H. A. 《Earth, Moon, and Planets》1997,78(1-3):45-51

Observations of comets in the 18-cm OH transitions offer a means to probe gas production, kinematics, and OH excitation in comets. We present initial results of OH observations of comet Hale-Bopp obtained with the NRAO 43 m antenna located in Greenbank, WV. Maps of the emission provide strong constraints on the amount of quenching of the inversion of the OH ground state Λ-doublet in the coma. Analysis of the total radio OH flux and maps of its radial brightness distribution indicate a quenched region on the order of ∼500,000 km during March and April 1997. This large value is generally consistent with previous observations of radio OH quenching in lower production rate comets when the high production rate of comet Hale-Bopp is considered. This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献   

Time-varying transformations for Hill–Clohessy–Wiltshire solutions in elliptic orbits     

Ryan E. Sherrill  Andrew J. Sinclair  S. C. Sinha  T. Alan Lovell 《Celestial Mechanics and Dynamical Astronomy》2014,119(1):55-73

The relative motion of chief and deputy satellites in close proximity with orbits of arbitrary eccentricity can be approximated by linearized time-periodic equations of motion. The linear time-invariant Hill–Clohessy–Wiltshire equations are typically derived from these equations by assuming the chief satellite is in a circular orbit. Two Lyapunov–Floquet transformations and an integral-preserving transformation are here presented which relate the linearized time-varying equations of relative motion to the Hill–Clohessy–Wiltshire equations in a one-to-one manner through time-varying coordinate transformations. These transformations allow the Hill–Clohessy–Wiltshire equations to describe the linearized relative motion for elliptic chief satellites.  相似文献   

The role of non-nation-state actors and side events in the international climate negotiations     

Heike Schroeder  Heather Lovell 《Climate Policy》2013,13(1):23-37

United Nations climate change conferences have attracted an increasing number and range of observer participants, often outnumbering national delegates. The interactions between the formal and informal spaces of climate governance at the Conference of the Parties (COP) are explored by investigating why non-nation state actors (NNSAs) attend them and by measuring to what extent official UN Side Events provide relevant information for the formal negotiations. Based on primary empirical research at recent COPs, it is found that 60–75% of Side Events have related directly to items under negotiation in the post-2012 climate negotiations. In this regard, Side Events that facilitate informal exchange between stakeholders not only provide input into the negotiations but also allow issues beyond the realm of the negotiations to be discussed, reflecting the scope of climate change. Although Side Events are an effective forum to exchange ideas and network, their current format and purpose as being events ‘on the side’ does not offer a sufficient framework for coordination between the work of NNSAs and the United Nations Framework Convention on Climate Change (UNFCCC) process.  相似文献   

Participatory action research approaches and methods: Connecting people, participation and place – Edited by Sara Kindon, Rachel Pain and Mike Kesby     

Sarah Lovell 《New Zealand geographer》2009,65(2):162-163

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Overview and current status of the VSOP mission     

J. E. J. Lovell  H. Hirabayashi  H. Kobayashi  Y. Murata  P. G. Edwards  G. A. Moellenbrock  S. Horiuchi  E. B. Fomalont  S. Kameno  K. M. Shibata 《New Astronomy Reviews》1999,43(8-10)

An overview and status report of the VLBI Space Observatory Programme is presented.  相似文献   

Three years of photometry of IM pegasi = HR8703     

J. A. Eaton  D. S. Hall  G. W. Henry  L. P. Lovell  C. A. Stephan  C. R. Chambliss  P. K. Detterline  H. J. Landis  H. Louth  T. R. Renner  D. R. Skillman 《Astrophysics and Space Science》1983,89(1):53-60

Differential photometry of this K1 IV–III p RS VNn-type binary in 1978–79, 1979–80, and 1980–81 at eight different observatories shows that the variability, discovered orignally by Herbst, is periodic. The mean of three different determinations of the photometric period was 24^d.39±-0^d.03, about 1% shorter than the orbital period of 24^d.649 determined spectroscopically by Harper. The total range observed during these three years was 5 ^m .60<V<5 ^m .85. The light curve was nearly sinusoidal but always noticeably asymmetric, with the sense reversing sometime between 1979–80 and 1980–81.  相似文献   

Laboratory studies of the electrical and fluid flow properties of porous media     

P.D. Jackson  M.A. Lovell  J.M. Waring  S.P. Hassett 《Marine and Petroleum Geology》1989,6(4)

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