Nina Tetzlaff, Baha Dinçel, Ralph Neuhäuser(Jena)

Transcription

1 Nina Tetzlaff, Baha Dinçel, Ralph Neuhäuser(Jena) Bonn workshop spring 2014 Wednesday, 05 March 2014

2 Outline 1. Introduction 2. PSR J Other Examples 4. Conclusions

3 Introduction

4 Introduction Binary supernova scenario(bss, Blaauw 1961) primary star of a massive close binary system experiences supernova companion becomes a runaway star(velocity up to orbital velocity) neutron star receives a kick velocity due to asymmetry of the supernova Arzoumanian et al Hobbs et al Histogram: observations Distribution of spatial velocities for neutron stars (figure from Hobbs et al. 2005).

5 Introduction We performed a systematic search for birth places of all young nearby neutron stars with known proper motion and distance kinematicage τ kin givesbetterestimateof thetrueneutronstarage than spin-downage τ char suitable to test neutron star cooling curves (cooling mechanism and composition of neutron star matter) Courtesy J. Pons constraints on the equation-of-state of matter under extreme conditions T eff, : effectivetemperatureseenbyobserver symbols: characteristicages

6 PSR J (with V. V. Kovtyukh, Odessa)

7 PSR J characteristic age: 4.92 Myr detected in X-rays, but only little thermal contribution (power law already fits spectrum well, Becker et al. 2004) 3σ upper limits for hot polar cap Cooling curves from J. Pons for different magnetic field strengths ( G, frombottomto top) for whole surface green: PSR J blue: characteristic ages red: kinematic ages (with temperature uncertainties)

8 PSR J possible birth associations/clusters nearby and very recent or more distantand a fewmyrago only one convincing former companioncandidate: HIP (G0Ia) supports origin in small clusterstock 7, 3.0 ±0.6 Myrago

9 PSR J HIP vsini= 29.0 ±2.3 km/s consistent evolutionaryage: 20 ±4 Myr consistentwithage of Stock 7 spectra in ELODIE archive available (Observatoire de Haute-Provence) flighttime: 3.0 ±0.6 Myr

10 PSR J HIP vsini= 29.0 ±2.3 km/s consistent evolutionaryage: 20 ±4 Myr consistentwithage of Stock 7 spectra in ELODIE archive available (Observatoire de Haute-Provence) abundances not inconsistent with supernova in a former binary (high N, Li, r process elements) flighttime: 3.0 ±0.6 Myr

11 PSR J Implication: progenitormass: M lowerlimit: at least equalto massof fcc, upperlimit: lowerage limitof parentclusterstock 7, Myr consistentwiththatitmustbehigherthanmostmassive presentclustermember: HD 15239, B2.5:Vn shell, Moffat& Vogt 1973, Abt et al. 1980, hence ~ 7-8 M, Schmidt- Kaler1982, Hohle et al. 2010) massratioof formerbinarysystem: m 2 /m 1 > 0.4 near-zeroradial velocityof NS yields3d velocityof i= 87 ±11 deg km/s and

12 Other Examples

13 Other Examples RX J : bornin Upper Scorpius(US), ~0.5 Myrago, presentsn positionwrtsun: ~155 pc, l~350, b~19 near-zero radial velocity consistent with observed bow shock (van Kerkwijk& Kulkarni 2001) Upper Scorpius RX J

14 Other Examples RX J : bornin Upper Scorpius(US), ~0.5 Myrago, present SN position wrt Sun: ~155 pc, l~350, b~19 Upper Scorpius +30 RX J : nine possible birth associations(due to large distance error for the neutron star) best formercompanioncandidate: HIP (B0II/III) thenoriginatedfromtrumpler ± 0.2 Myrago Trumpler 10 HIP presentsn positionwrtsun: ~380pc, l~260, RX J b~2.4 RX J

15 Other Examples RX J : bornin Upper Scorpius(US), ~0.5 Myrago, present SN position wrt Sun: ~155 pc, l~350, b~19 Upper Scorpius +30 RX J : bornin Tr10, fcchip 43158, ~1 Myrago, present SN position wrt Sun: ~380 pc, l~260, b~2.4 Trumpler 10 PSR J : bornin AntliaSNR, ~1.2 Myrago best candidatens becausehip supports origin in Antlia SNR afterwardsmeasuredrv (G. Torres, Arizona) for fcc consistent with predicted value presentsn/snr positionwrtsun: ~140 pc, l~270.4, b~19.2 HIP RX J RX J

16 All 20 Neutron Stars Investigated in Detail 12 of themprobablyformedwithin500 pcfromthesun 7 neutron stars possibly born in the Solar neighbourhood (Scorpius-Centaurus, younglocalassociations) contributionto 60 Fe? Knie et al Fitoussi et al previouslyidentifiedpair PSR B /ς Ophiuchi(Hoogerwerfet al. 2001) not recovered due to improved parallax of neutron star former companion candidates found for 11 neutron stars

17 All 20 Neutron Stars Investigated in Detail Abbreviations: Cam: Camelopardalis; Cas: Cassiopeia; Cen: Centaurus; Cyg: Cygnus; Ori: Orion; Sco: Scorpius; Ser: Serpens; Sgr: Sagittarius; Tr: Trumpler; US: Upper Scorpius +90 young clusters massive associations young local associations supernova remnants(snrs) +45 galactic latitude Cam OB1 Cas Cyg OB9 Antlia SNR US Ser OB1 Sco-Cen +30 Monogem Ring +15 Sco OB4 Cen OB1 Tr 10 Sgr OB1 Vela SNR Ori OB1a galactic longitude -60

18 All 20 Neutron Stars Investigated in Detail Abbreviations: Cam: Camelopardalis; Cas: Cassiopeia; Cen: Centaurus; Cyg: Cygnus; Ori: Orion; Sco: Scorpius; Ser: Serpens; Sgr: Sagittarius; Tr: Trumpler; US: Upper Scorpius +90 young clusters massive associations young local associations supernova remnants(snrs) +45 Cam OB1 Cas Cyg OB9 Antlia SNR US Ser OB1 Sco-Cen +30 Monogem Ring +15 Sco OB4 Cen OB1 Tr 10 Sgr OB1 Vela SNR Ori OB1a Neutron stars: (symbols indicate present positions) RX J RX J (with HIP 43158)

19 All 20 Neutron Stars Investigated in Detail Abbreviations: Cam: Camelopardalis; Cas: Cassiopeia; Cen: Centaurus; Cyg: Cygnus; Ori: Orion; Sco: Scorpius; Ser: Serpens; Sgr: Sagittarius; Tr: Trumpler; US: Upper Scorpius +90 young clusters massive associations young local associations supernova remnants(snrs) +45 Cam OB1 Cas Cyg OB9 Antlia SNR US Ser OB1 Sco-Cen +30 Monogem Ring +15 Sco OB4 Cen OB1 Tr 10 Sgr OB1 Vela SNR Ori OB1a Neutron stars: (symbols indicate present positions) RX J RX J (with HIP 43158) PSR B (with ς Ophiuchi)

20 All 20 Neutron Stars Investigated in Detail Abbreviations: Cam: Camelopardalis; Cas: Cassiopeia; Cen: Centaurus; Cyg: Cygnus; Ori: Orion; Sco: Scorpius; Ser: Serpens; Sgr: Sagittarius; Tr: Trumpler; US: Upper Scorpius +90 young clusters massive associations young local associations supernova remnants(snrs) +45 Cam OB1 Cas Cyg OB9 Antlia SNR US Ser OB1 Sco-Cen +30 Monogem Ring +15 Sco OB4 Cen OB1 Tr 10 Sgr OB1 Vela SNR Ori OB1a Neutron stars: (left to right; symbols indicate present positions) PSR J PSR J PSR J PSR J PSR B PSR J RX J PSR J RX J (with HIP 43158) RX J Vela Pulsar -60 PSR J PSR J (with HIP 63049, 61744) PSR J PSR J PSR J PSR J PSR J Geminga Pulsar

21 All 20 Neutron Stars Investigated in Detail Abbreviations: Cam: Camelopardalis; Cas: Cassiopeia; Cen: Centaurus; Cyg: Cygnus; Ori: Orion; Sco: Scorpius; Ser: Serpens; Sgr: Sagittarius; Tr: Trumpler; US: Upper Scorpius +90 young clusters massive associations young local associations supernova remnants(snrs) +45 Cam OB1 Cas Cyg OB9 Antlia SNR US Ser OB1 Sco-Cen +30 Monogem Ring +15 Sco OB4 Cen OB1 Tr 10 Sgr OB1 Vela SNR Ori OB1a Neutron stars: (left to right; symbols indicate present positions) PSR J PSR J PSR J (with HIP 99580) PSR J RX J (with HIP 89394) PSR J PSR B PSR J RX J (with HIP 43158) RX J Vela Pulsar -60 PSR J PSR J (with HIP 63049, 61744) PSR J (with HIP 47155) -45 PSR J PSR J PSR J PSR J (with HIP 13962) Geminga Pulsar

22 All 20 Neutron Stars Investigated in Detail direction of kick wrt galactic plane Very preliminary small sample!

23 Conclusions and Outlook

24 Conclusions and Outlook itiswell feasibleto determinethebirthplaceof a neutronstarand its kinematic age if the observables are sufficiently precise in many cases no unique birth place, hence other indicators necessary, e.g. former companion(runaway star) confirmationof radial velocity, e.g. bymeansof a bowshock 40 former companion candidates proposed for follow-up observations indications for evolution in a former binary system, indications for a past supernova event (such as in thecasepsr J / HIP 13962) weprovide3d velocitiesthatcanbeusedto investigatethealignment betweenkick and magneticaxesorkick and spinaxes

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