The asteroid lightcurve database

Warner, Brian D.; Harris, Alan W.; Pravec, Petr

doi:10.1016/j.icarus.2009.02.003

Cited by 492 publications

(554 citation statements)

References 21 publications

Supporting

Mentioning

521

Contrasting

Unclassified

Order By: Relevance

“…For this reason we belive the phase curve should be shifted downwards by about 0.45 mag, so that it coincides with our photometric measurements, thus a new value for the absolute magnitude is H = 24.29 mag. We note that the G = 0.2 obtained from our fit is close to the average value of 0.24 derived for S-type asteroids (Warner et al 2009). It is difficult to estimate the accuracy of the H value, so we assume the maximum systematic uncertainty of H to be 0.5 mag, thus the absolute magnitude for 2014 NL52 becomes H = 24.3 ± 0.5 mag.…”

Section: Phase Curve and Sizesupporting

confidence: 88%

“…All lightcurves simulated at α = 58 • and A = 0.6 mag had two maxima and two minima per period. This let us believe the P 2 solution represents the true period of 2014 NL52 so that we assign it a reliability code U = 2+ (Warner et al 2009). We did not attempt to fold the 20 and 29 July data because the 3σ uncertainty in the derived synodic period, after 9 days, would lead to the uncertainty in the rotation phase as large as 6 rotations.…”

Section: Rotation Periodmentioning

confidence: 95%

See 1 more Smart Citation

First EURONEAR NEA discoveries from La Palma using the INT★

Văduvescu

Hudin²,

Tudor

et al. 2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Since 2006, the EURONEAR project has been contributing to the research of near Earth asteroids (NEAs) within an European network. One of the main aims is the amelioration of the orbits of NEAs, and starting in February 2014 we focus on the recovery of one-opposition NEAs using the Isaac Newton Telescope (INT) in La Palma in override mode. Part of this NEA recovery project, since June 2014 EURONEAR serendipitously started to discover and secure the first NEAs from La Palma and using the INT, thanks to the team-work including amateurs and students who promptly reduce the data, report discoveries and secure new objects recovered with the INT and few other telescopes from the EURONEAR network. Five NEAs were discovered with the INT, including 2014 LU14, 2014 NL52 (one very fast rotator), 2014 OL339 (the fourth known Earth quasi-satellite), 2014 SG143 (a quite large NEA) and 2014 VP. Another very fast moving NEA was discovered but was unfortunately lost due to lack of follow-up time. Additionally, another 14 NEA candidates were identified based on two models, all being rapidly followed-up using the INT and another 11 telescopes within the EURONEAR network. They include one object discovered by Pan-STARRS, two Mars crossers, two Hungarias, one Jupiter trojan, and other few inner MBAs. Using the INT and Sierra Nevada 1.5 m for photometry, then the Gran Telescopio de Canarias (GTC) for spectroscopy, we derived the very rapid rotation of 2014 NL52, then its albedo, magnitude, size, and its spectral class. Based on the total sky coverage in dark conditions, we evaluate the actual survey discovery rate using 2-m class telescopes. One NEA is possible to be discovered randomly within minimum 2.8 square degrees and maximum 5.5 square degrees. These findings update our past statistics, being based on double sky coverage and taking into account the recent increase in discovery.

show abstract

Section: Phase Curve and Sizesupporting

confidence: 88%

Section: Rotation Periodmentioning

confidence: 95%

First EURONEAR NEA discoveries from La Palma using the INT★

Văduvescu

Hudin²,

Tudor

et al. 2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…Statistical considerations in this section are based on the Minor Planer Center Lightcurve Database (LCDB, Warner et al 2009Warner et al , updated 2016 September 5) using a sample of the ∼1200 brightest main belt asteroids (those with absolute magnitudes H≤11 mag, Fig. 1), 1 which translates to diameters down to 12-37 km, depending on albedo (after MPC conversion table 2 ).…”

Section: Observing and Modelling Biases In Asteroid Studiesmentioning

confidence: 99%

Photometric survey, modelling, and scaling of long-period and low-amplitude asteroids

Marciniak

Bartczak

Müller

et al. 2018

A&A

View full text Add to dashboard Cite

Context. The available set of spin and shape modelled asteroids is strongly biased against slowly rotating targets and those with low lightcurve amplitudes. This is due to the observing selection effects. As a consequence, the current picture of asteroid spin axis distribution, rotation rates, radiometric properties, or aspects related to the object's internal structure might be affected too. Aims. To counteract these selection effects, we are running a photometric campaign of a large sample of main belt asteroids omitted in most previous studies. Using least chi-squared fitting we determined synodic rotation periods and verified previous determinations. When a dataset for a given target was sufficiently large and varied, we performed spin and shape modelling with two different methods to compare their performance. Methods. We used the convex inversion method and the non-convex SAGE algorithm, applied on the same datasets of dense lightcurves. Both methods search for the lowest deviations between observed and modelled lightcurves, though using different approaches. Unlike convex inversion, the SAGE method allows for the existence of valleys and indentations on the shapes based only on lightcurves. Results. We obtain detailed spin and shape models for the first five targets of our sample: (159) Aemilia, (227) Philosophia, (329) Svea, (478) Tergeste, and (487) Venetia. When compared to stellar occultation chords, our models obtained an absolute size scale and major topographic features of the shape models were also confirmed. When applied to thermophysical modelling, they provided a very good fit to the infrared data and allowed their size, albedo, and thermal inertia to be determined. Conclusions. Convex and non-convex shape models provide comparable fits to lightcurves. However, some non-convex models fit notably better to stellar occultation chords and to infrared data in sophisticated thermophysical modelling (TPM). In some cases TPM showed strong preference for one of the spin and shape solutions. Also, we confirmed that slowly rotating asteroids tend to have higher-than-average values of thermal inertia, which might be caused by properties of the surface layers underlying the skin depth.

show abstract

“…Using the colour derived from the reflectance spectra and the observing geometry of the observations, we measure an absolute magnitude of H V = 14.30±0.08 for asteroid 7343. A G-value (Bowell et al 1989) of 0.24 ± 0.11 was used, typical for S-type asteroids (Warner et al 2009). The large uncertainty in the absolute magnitude is dominated by the uncertainty in the G-value used.…”

Section: Lightcurve Observationsmentioning

confidence: 99%

Physical and dynamical characterisation of the unbound asteroid pair 7343-154634

Duddy

Lowry

Wolters

et al. 2012

A&A

View full text Add to dashboard Cite

Context. Models have shown that asteroids can undergo fission if their rate of rotation is steadily increased. The forces acting to pull the asteroid apart exceed the material strength and gravitational force holding the asteroid together and material can escape from the surface of the asteroid. Initially forming a binary asteroid system, the components are capable of decoupling at low relative velocity from their mutual orbit if their mass ratio is less than 0.2. A number of asteroids with very similar orbital elements have been shown to have had very recent (<1 Myr) encounters at distances smaller than the Hill sphere radius of the larger of the asteroids. The mass ratio of the asteroids in each pair is estimated to be less than 0.2, suggesting that these unbound pairs are the result of rotational fission. Aims. We determine whether the asteroids in one such unbound pair, (7343) Ockeghem and (154 634) 2003 XX28, share a common composition, indicative of asteroids formed from a common parent and further constrain a likely formation age for this pair. Methods. We have obtained spectroscopic observations of each asteroid covering the wavelength range 0.45 to 1.0 microns. Using thermal observations we have measured the size and albedo of (7343) Ockeghem. Combined with optical lightcurve data of both asteroids, we have constrained the size and density of the asteroids and estimated the strength of the Yarkovsky force experienced by both. This improved physical information has been used in new dynamical simulations of the asteroids' orbits to better constrain a formation time of this pair. Results. We find that the asteroids have very similar spectra consistent with an S-type taxonomy. The geometric albedo of (7343) Ockeghem, 0.20 ± 0.06 is consistent with this classification. The mass ratio range of the asteroids assuming an equal density, 0.007 to 0.065, is consistent with models of unbound asteroid pair formation. A new dynamical analysis has indicated that an absolute lower limit for the age of this pair is 400 kyr with a more likely age around 560 kyr, lower than a previous estimate of 800 kyr.

show abstract

The asteroid lightcurve database

Cited by 492 publications

References 21 publications

First EURONEAR NEA discoveries from La Palma using the INT★

First EURONEAR NEA discoveries from La Palma using the INT★

Photometric survey, modelling, and scaling of long-period and low-amplitude asteroids

Physical and dynamical characterisation of the unbound asteroid pair 7343-154634

Contact Info

Product

Resources

About