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postgraduate thesis: Interacting binary jets in L1551 IRS 5 protobinary system

TitleInteracting binary jets in L1551 IRS 5 protobinary system
Authors
Advisors
Advisor(s):Lim, JJL
Issue Date2012
PublisherThe University of Hong Kong (Pokfulam, Hong Kong)
AbstractRodr??guez et al. (2003b) used Very Large Array (VLA) in addition of Pie Town antenna (PT antenna) to observe the low mass protostellar system, L1551 IRS 5 at 3.5 cm. Their radio map showed two main results: a number of knots along the two extend radio jets driven from L1551 IRS 5 and the southern jet shows a peculiar bend at about 0.006 to the southwest of the driving source. To inves- tigate how the knots formed and what causes the bend in southern jet, I found three data sets reliable to make the maps from the VLA online data archive comprising 1994, 2002 and 2003. The 3.5 cm radio continuum maps of three epochs showed similar jets structure. I denoted the knots as RK A, B, C, D, E, F and G. For interpreting the nature of the knots seen in both jets and variations in the intensity/structure of the southern jet, I make the difference maps for multi-epoch comparison. There are no significant residuals (> 4_) for above-mentioned knots. We measure the velocities of the RKs relative to RK A: RK C (19 ± 13 kms?1), RK D (7.5 ± 4.7 kms?1 between epoch 1994 and 2002, 85 ± 20 kms?1 between epoch 2002 and 2003), RK E (72 ± 24 kms?1) and RK G (24 ± 32 kms?1). And the intrinsic velocity of RK B relative to southern protostar is 3.8 ± 2.8 kms?1. All of them are insignificant (< 4 _). However, I detected a positive residual with highly significant (> 6_) in all difference maps. I denoted it as RK H. And I obtained a significant proper motion of RK H (128 ± 18 kms?1). RK B, C, D, E, F and G are not likely formed by enhancement in mass loss or internal shock because their 4_ upper limit velocities are much slower than jet velocities of their corresponding jet. They can be interpreted by either the model of interaction of the binary jets or interaction with ambience cloudlets. Since the flux density of RK H is roughly constant within 1_ so that it is not likely formed by enhancement in mass loss but it can be explained by internal shock.
DegreeMaster of Philosophy
SubjectAstrophysical jets.
Dept/ProgramPhysics

 

DC FieldValueLanguage
dc.contributor.advisorLim, JJL-
dc.contributor.authorLeung, Ka-wing-
dc.contributor.author梁家榮-
dc.date.issued2012-
dc.description.abstractRodr??guez et al. (2003b) used Very Large Array (VLA) in addition of Pie Town antenna (PT antenna) to observe the low mass protostellar system, L1551 IRS 5 at 3.5 cm. Their radio map showed two main results: a number of knots along the two extend radio jets driven from L1551 IRS 5 and the southern jet shows a peculiar bend at about 0.006 to the southwest of the driving source. To inves- tigate how the knots formed and what causes the bend in southern jet, I found three data sets reliable to make the maps from the VLA online data archive comprising 1994, 2002 and 2003. The 3.5 cm radio continuum maps of three epochs showed similar jets structure. I denoted the knots as RK A, B, C, D, E, F and G. For interpreting the nature of the knots seen in both jets and variations in the intensity/structure of the southern jet, I make the difference maps for multi-epoch comparison. There are no significant residuals (> 4_) for above-mentioned knots. We measure the velocities of the RKs relative to RK A: RK C (19 ± 13 kms?1), RK D (7.5 ± 4.7 kms?1 between epoch 1994 and 2002, 85 ± 20 kms?1 between epoch 2002 and 2003), RK E (72 ± 24 kms?1) and RK G (24 ± 32 kms?1). And the intrinsic velocity of RK B relative to southern protostar is 3.8 ± 2.8 kms?1. All of them are insignificant (< 4 _). However, I detected a positive residual with highly significant (> 6_) in all difference maps. I denoted it as RK H. And I obtained a significant proper motion of RK H (128 ± 18 kms?1). RK B, C, D, E, F and G are not likely formed by enhancement in mass loss or internal shock because their 4_ upper limit velocities are much slower than jet velocities of their corresponding jet. They can be interpreted by either the model of interaction of the binary jets or interaction with ambience cloudlets. Since the flux density of RK H is roughly constant within 1_ so that it is not likely formed by enhancement in mass loss but it can be explained by internal shock.-
dc.languageeng-
dc.publisherThe University of Hong Kong (Pokfulam, Hong Kong)-
dc.relation.ispartofHKU Theses Online (HKUTO)-
dc.rightsThe author retains all proprietary rights, (such as patent rights) and the right to use in future works.-
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.source.urihttp://hub.hku.hk/bib/B4775302X-
dc.subject.lcshAstrophysical jets.-
dc.titleInteracting binary jets in L1551 IRS 5 protobinary system-
dc.typePG_Thesis-
dc.identifier.hkulb4775302-
dc.description.thesisnameMaster of Philosophy-
dc.description.thesislevelMaster-
dc.description.thesisdisciplinePhysics-
dc.description.naturepublished_or_final_version-
dc.identifier.doi10.5353/th_b4775302-
dc.date.hkucongregation2012-

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