The double explosion of SN 2009ip in 2012 raises questions about our understanding of the late stages of massive star evolution. Here we present a comprehensive study of SN 2009ip during its ...remarkable rebrightenings. High-cadence photometric and spectroscopic observations from the GeV to the radio band obtained from a variety of ground-based and space facilities (including the Very Large Array, Swift, Fermi, Hubble Space Telescope, and XMM) constrain SN 2009ip to be a low energy (E ~ 10 super(50) erg for an ejecta mass ~0.5 M sub(middot in circle)) and asymmetric explosion in a complex medium shaped by multiple eruptions of the restless progenitor star. Most of the energy is radiated as a result of the shock breaking out through a dense shell of material located at ~5 x 10 super(14)cm with M ~ 0.1 M sub(middot in circle), ejected by the precursor outburst ~40 days before the major explosion. We interpret the NIR excess of emission as signature of material located further out, the origin of which has to be connected with documented mass-loss episodes in the previous years. Our modeling predicts bright neutrino emission associated with the shock break-out if the cosmic-ray energy is comparable to the radiated energy. We connect this phenomenology with the explosive ejection of the outer layers of the massive progenitor star, which later interacted with material deposited in the surroundings by previous eruptions. Future observations will reveal if the massive luminous progenitor star survived. Irrespective of whether the explosion was terminal, SN 2009ip brought to light the existence of new channels for sustained episodic mass loss, the physical origin of which has yet to be identified.
Algunos ejercicios de natación alteran la rotación del eje longitudinal del cuerpo. Este estudio determinó las diferencias y la simetría de la rotación del hombro y la cadera causada por diferentes ...ejercicios. En un diseño transversal, 16 nadadores entrenados realizaron seis protocolos diferentes de nado a crol: i) no respiración (NR); ii) respiración derecha (RD); iii) un brazo extendido y respiración derecha (ERD) o iv) izquierda (ERI); v) un brazo pegado al cuerpo y respiración derecha (CRD) o vi) izquierda (CRI). Los ejercicios se registraron en vídeo con dos cámaras frontales y los ángulos se midieron mediante Kinovea®. El ANOVA de dos vías exploró la interacción protocolos-ejercicio. Las diferencias entre el lado del brazo ejecutor (BE) y el no ejecutor (BNE) se compararon mediante pruebas t de muestras pareadas. Los hombros rotaron más que las caderas y alcanzaron antes la máxima rotación. La respiración aumentó la rotación en ~7-12˚. CRD y CRI mostraron rangos de rotación más bajos que los otros protocolos, pero obtuvieron asimetrías significativas entre el lado ejecutor (hombro: 8-19˚; cadera: 12-17˚) y no ejecutor (hombro: 66-77˚; cadera: 51-68˚). CRD y CRI mostraron rangos de rotación similares a los de la natación normal, pero obtuvieron un tiempo de ciclo de brazada diferente (1.5 s vs. 1.3 s). Los cambios entre la rotación de hombros y caderas no fueron homogéneos y se vieron especialmente propiciados por los ejercicios de natación, sobre todo al respirar. Los entrenadores deberían reconsiderar la inclusión de estos ejercicios en programas de natación
The double explosion of SN 2009ip in 2012 raises questions about our understanding of the late stages of massive star evolution. Here we present a comprehensive study of SN 2009ip during its ...remarkable rebrightenings. High-cadence photometric and spectroscopic observations from the GeV to the radio band obtained from a variety of ground-based and space facilities (including the Very Large Array, Swift, Fermi, Hubble Space Telescope, and XMM) constrain SN 2009ip to be a low energy (E approximating 10(exp 50) ergs for an ejecta mass approximating 0.5 M solar mass) and asymmetric explosion in a complex medium shaped by multiple eruptions of the restless progenitor star. Most of the energy is radiated as a result of the shock breaking out through a dense shell of material located at approximately 5 times 10 (exp 14) cm with M approximating 0.1 solar mass, ejected by the precursor outburst approximately 40 days before the major explosion. We interpret the NIR (Near Infrared) excess of emission as signature of material located further out, the origin of which has to be connected with documented mass-loss episodes in the previous years. Our modeling predicts bright neutrino emission associated with the shock break-out if the cosmic-ray energy is comparable to the radiated energy. We connect this phenomenology with the explosive ejection of the outer layers of the massive progenitor star, which later interacted with material deposited in the surroundings by previous eruptions. Future observations will reveal if the massive luminous progenitor star survived. Irrespective of whether the explosion was terminal, SN 2009ip brought to light the existence of new channels for sustained episodic mass loss, the physical origin of which has yet to be identified.
The 2012 explosion of SN2009ip raises questions about our understanding of the late stages of massive star evolution. Here we present a comprehensive study of SN2009ip during its remarkable ...re-brightening(s). High-cadence photometric and spectroscopic observations from the GeV to the radio band obtained from a variety of ground-based and space facilities (including the VLA, Swift, Fermi, HST and XMM) constrain SN2009ip to be a low energy (E~ 10^50 erg for an ejecta mass ~ 0.5 Msun) and likely asymmetric explosion in a complex medium shaped by multiple eruptions of the restless progenitor star. Most of the energy is radiated as a result of the shock breaking out through a dense shell of material located at 5x10^14 cm with M~0.1 Msun, ejected by the precursor outburst ~40 days before the major explosion. We interpret the NIR excess of emission as signature of dust vaporization of material located further out (R>4x 10^15 cm), the origin of which has to be connected with documented mass loss episodes in the previous years. Our modeling predicts bright neutrino emission associated with the shock break-out if the cosmic ray energy is comparable to the radiated energy. We connect this phenomenology with the explosive ejection of the outer layers of the massive progenitor star, that later interacted with material deposited in the surroundings by previous eruptions. Future observations will reveal if the luminous blue variable (LBV) progenitor star survived. Irrespective of whether the explosion was terminal, SN2009ip brought to light the existence of new channels for sustained episodic mass-loss, the physical origin of which has yet to be identified.
PDF
