Mirror and Point Symmetries in a Ballistic Jet From a Binary System

Raga, A. C.; Esquivel, A.; Velázquez, P. F.; Cantó, J.; Haro-Corzo, S.; Riera, A.; Rodríguez-González, A.

doi:10.1088/0004-637x/707/1/l6

Cited by 50 publications

(69 citation statements)

References 19 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Anglada et al (2007), using the formulation given by Masciadri & Raga (2002), analyze the extreme cases where the dominant effect is either the orbital motion of the jet source in a binary system, or the precession of the ejection axis of the jet because of tidal interactions between the disk where the jet originates and a companion star. Here, we develop the work of Raga et al (2009b), and we consider a physical system, in which both the orbital motion and precession can be present simultaneously, to fit the HH 30 jet and counterjet wiggling shape.…”

Section: Jet Wigglingmentioning

confidence: 99%

The Counterjet of Hh 30: New Light on Its Binary Driving Source

Estalella

López

Anglada

et al. 2012

The Astronomical Journal

View full text Add to dashboard Cite

We present new [S ii] images of the Herbig-Haro (HH) 30 jet and counterjet observed in 2006, 2007, and 2010 that, combined with previous data, allowed us to measure with improved accuracy the positions and proper motions of the jet and counterjet knots. Our results show that the motion of the knots is essentially ballistic, with the exception of the farthest knots, which trace the large-scale "C"-shape bending of the jet. The observed bending of the jet can be produced by a relative motion of the HH 30 star with respect to its surrounding environment, caused either by a possible proper motion of the HH 30 star, or by the entrainment of environment gas by the red lobe of the nearby L1551-IRS5 outflow. Alternatively, the bending can be produced by the stellar wind from a nearby classical T Tauri star, identified in the Two Micron All Sky Survey catalog as J04314418+181047. The proper motion velocities of the knots of the counterjet show more variations than those of the jet. In particular, we identify two knots of the counterjet that have the same kinematic age but whose velocities differ by almost a factor of two. Thus, it appears from our observations that counterjet knots launched simultaneously can be ejected with very different velocities. We confirm that the observed wiggling of the jet and counterjet arises from the orbital motion of the jet source in a binary system. Precession, if present at all, is of secondary importance in shaping the jet. We derive an orbital period of τ o = 114 ± 2 yr and a mass function of mμ 3 c = 0.014 ± 0.006 M . For a mass of the system of m = 0.45 ± 0.04 M (the value inferred from observations of the CO kinematics of the disk), we obtain a mass of m j = 0.31 ± 0.04 M for the jet source, a mass of m c = 0.14 ± 0.03 M for the companion, and a binary separation of a = 18.0 ± 0.6 AU. This binary separation coincides with the value required to account for the size of the inner hole observed in the disk, which has been attributed to tidal truncation in a binary system.

show abstract

Section: Jet Wigglingmentioning

confidence: 99%

The Counterjet of Hh 30: New Light on Its Binary Driving Source

Estalella

López

Anglada

et al. 2012

The Astronomical Journal

View full text Add to dashboard Cite

show abstract

“…As we have pointed out in the past (Masciadri & Raga 2002;Raga et al 2009), an orbital motion of the jet source can result in mirror symmetries of the outflow lobes. However, the relatively low orbital velocities possible for the sources of observed mirror-symmetric pPNs cannot be responsible for the large angular deviations of their outflow lobes (Velázquez et al 2013;Riera et al 2014).…”

Section: Discussionmentioning

confidence: 75%

“…For orbital periods less than the precession period, these authors found that mirror symmetry is observed close to the central source with respect to the orbital plane, while point-symmetric morphologies prevail at larger distances (Masciadri & Raga 2002;Raga et al 2009). The influence of the orbital motion on the line emission of these objects was analyzed by Haro-Corzo et al (2009).…”

Section: Introductionmentioning

confidence: 98%

An Asymmetric Jet-Launching Model for the Protoplanetary Nebula CRL 618

Velázquez

Riera

Raga

et al. 2014

ApJ

View full text Add to dashboard Cite

We propose an asymmetrical jet-ejection mechanism in order to model the mirror symmetry observed in the lobe distribution of some protoplanetary nebulae (pPNs), such as the pPN CRL 618. Three-dimensional hydrodynamical simulations of a precessing jet launched from an orbiting source were carried out, including an alternation in the ejections of the two outflow lobes, depending on which side of the precessing accretion disk is hit by the accretion column from a Roche lobe-filling binary companion. Both synthetic optical emission maps and position-velocity diagrams were obtained from the numerical results with the purpose of carrying out a direct comparison with observations. Depending on the observer's point of view, multipolar morphologies are obtained that exhibit a mirror symmetry at large distances from the central source. The obtained lobe sizes and their spatial distributions are in good agreement with the observed morphology of the pPN CRL 618. We also obtain that the kinematic ages of the fingers are similar to those obtained in the observations.

show abstract

“…Alternatively, the mirror-symmetry (or multipolar geometry) may be caused by the orbital motion of a binary system (i.e., the jet source is moving in an orbit around a stellar companion) (Haro-Corzo et al 2009;Raga et al 2009). Haro-Corzo et al (2009) computed three-dimensional hydrodynamical simulations of a jet launched from the secondary star of a binary system.…”

Section: Discussionmentioning

confidence: 99%

STIS optical spectroscopy of the lobes of CRL 618

Riera

Raga

Velázquez

et al. 2011

A&A

Self Cite

View full text Add to dashboard Cite

Context. Many proto-planetary nebulae show collimated structures sometimes showing multiple outflows. Aims. We present the results of new optical spectroscopic observations (both medium (with a dispersion of 0.56 Å pixel −1 ) and low (2.73 and 4.92 Å pixel −1 for the G430L and G750L gratings) spectral resolution) of the lobes of the proto-planetary nebula CRL 618 obtained with the Space Telescope Imaging Spectrograph on board of the Hubble Space Telescope. Methods. We analyse the density structure and the excitation conditions of the lobes of CRL 618. The spectra obtained at medium spectral resolution (∼50 km s −1 ) allow us to quote the fraction of unscattered (intrinsic) Hα emission. We have also obtained dereddened emission line ratios of several features from the low spectral resolution spectra. Results. We find that most of the analysed line ratios are reproduced by planar shocks moving through a dense medium (with preshock densities ∼10 4 cm −3 ) with shock velocities from 30 to 40 km s −1 (except the [O III]/Hβ line ratios which require shock velocities of 80 to 90 km s −1 ). We find that the [S II]-weighted ionization fraction ranges from 0.015 to 0.06. The total densities derived from the electron density and the ionization fraction are ∼10 5 to 10 6 cm −3 . Conclusions. We conclude that the spectra of the lobes of CRL 618 can be margially reproduced by steady plane-parallel shock models for shock velocities which are significantly lower than the velocities at which the jet moves outwards (∼200 km s −1 ). These results are consistent with the predictions of a jet with a variable ejection velocity. The mirror-symmetry, the luminosity asymmetry between both lobes and the ejection velocity variability suggest that its central source may host a binary system.

show abstract

Mirror and Point Symmetries in a Ballistic Jet From a Binary System

Cited by 50 publications

References 19 publications

The Counterjet of Hh 30: New Light on Its Binary Driving Source

The Counterjet of Hh 30: New Light on Its Binary Driving Source

An Asymmetric Jet-Launching Model for the Protoplanetary Nebula CRL 618

STIS optical spectroscopy of the lobes of CRL 618

Contact Info

Product

Resources

About