adsabs/AstroCLIMB huggingface dataset:
Paper: In LIGO’s Sight? Vigorous Coherent Gravitational Waves from Cooled Collapsar Disks
Authors: Ore Gottlieb, Amir Levinson, Yuri Levin
Figure caption: 3D renderings illustrate the logarithmic mass density (in cgs) of post-merger accretion disks. The length scale can be measured with respect to the size of the BH in the center. (a) The early formation stages of the disk (∼10 ms) feature high-density spiral arms resulting from the disrupted NS. (b) As the matter axisymmetrized, the compact accretion disk becomes homogeneous. The full movie showcasing the evolution of the post-merger accretion disk is available at http://www.oregottlieb.com/disk_gw.html or on Zenodo (doi:10.5281/zenodo.13139529). (c–f) Edge-on (red) and face-on (blue) spectra for model B, with different rows depicting the spectra at various times. The dotted black lines represent the CE sensitivity curve.
Paper: In LIGO’s Sight? Vigorous Coherent Gravitational Waves from Cooled Collapsar Disks
Authors: Ore Gottlieb, Amir Levinson, Yuri Levin
Figure caption: The GW luminosity as a function of time, L GW = dE GW/dt, illustrates that the GW power grows similarly in all models.
Paper: In LIGO’s Sight? Vigorous Coherent Gravitational Waves from Cooled Collapsar Disks
Authors: Ore Gottlieb, Amir Levinson, Yuri Levin
Figure caption: Cross (panels (a) and (c)) and plus (panels (b) and (d)) polarizations for face-on observers (panels (a) and (b)) and edge-on observers (panels (c) and (d)) feature two characteristic timescales. Short timescales, characterized by high variability, are dictated by the orbit of nonaxisymmetric density waves close to the BH. Modulations on longer timescales (∼0.1 s) in model Cc imply that modes at larger orbits contribute to the GW spectrum in extended disks. See also the animation on Zenodo–doi:10.5281/zenodo.13139529.
Paper: In LIGO’s Sight? Vigorous Coherent Gravitational Waves from Cooled Collapsar Disks
Authors: Ore Gottlieb, Amir Levinson, Yuri Levin
Figure caption: The spectra in model C as calculated using the quadrupole approximation (blue) and the Green’s function (red) for face-on observers.
Paper: Extended Shock Breakout and Early Circumstellar Interaction in SN 2024ggi
Authors: Manisha Shrestha, K. Azalee Bostroem, David J. Sand, Griffin Hosseinzadeh, Jennifer E. Andrews, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jeniveve Pearson, Jacob E. Jencson, M. J. Lundquist, Darshana Mehta, Aravind P. Ravi, Nicolás Meza Retamal, Stefano Valenti, Peter J. Brown, Saurabh W. Jha, Colin Macrie, Brian Hsu, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey Kwok, Nathan Smith, Michaela Schwab, Aidan Martas, Ricardo R. Munoz, Gustavo E. Medina, Ting S. Li, Paula Diaz, Daichi Hiramatsu, Brad E. Tucker, J. C. Wheeler, Xiaofeng Wang, Qian Zhai, Jujia Zhang, Anjasha Gangopadhyay, Yi Yang, Claudia P. Gutiérrez
Figure caption: Optical spectral sequence of SN 2024ggi going from +0.9 day (Zhai et al. 2024) to +12.6 days after the explosion. Spectra from different instruments are indicated by different colors, as indicated in the legend, with the phases indicated on the right. The early spectra show flash features that disappear by roughly +3.5 days. All spectra will be made available on WISeREP (https://www.wiserep.org).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Extended Shock Breakout and Early Circumstellar Interaction in SN 2024ggi
Authors: Manisha Shrestha, K. Azalee Bostroem, David J. Sand, Griffin Hosseinzadeh, Jennifer E. Andrews, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jeniveve Pearson, Jacob E. Jencson, M. J. Lundquist, Darshana Mehta, Aravind P. Ravi, Nicolás Meza Retamal, Stefano Valenti, Peter J. Brown, Saurabh W. Jha, Colin Macrie, Brian Hsu, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey Kwok, Nathan Smith, Michaela Schwab, Aidan Martas, Ricardo R. Munoz, Gustavo E. Medina, Ting S. Li, Paula Diaz, Daichi Hiramatsu, Brad E. Tucker, J. C. Wheeler, Xiaofeng Wang, Qian Zhai, Jujia Zhang, Anjasha Gangopadhyay, Yi Yang, Claudia P. Gutiérrez
Figure caption: High-resolution data from SALT HRS observed on MJD 60413.96 (+3.16 days) focused on the Na I D lines of the host galaxy and Milky Way. There are six different absorption features corresponding to Na I D1 and D2 lines for the Milky Way, the host galaxy, and an intervening cloud, shown by blue lines for different redshifts. The total equivalent width of these lines measured from all the high-resolution spectra was used to calculate the extinction toward SN 2024ggi.
Paper: Extended Shock Breakout and Early Circumstellar Interaction in SN 2024ggi
Authors: Manisha Shrestha, K. Azalee Bostroem, David J. Sand, Griffin Hosseinzadeh, Jennifer E. Andrews, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jeniveve Pearson, Jacob E. Jencson, M. J. Lundquist, Darshana Mehta, Aravind P. Ravi, Nicolás Meza Retamal, Stefano Valenti, Peter J. Brown, Saurabh W. Jha, Colin Macrie, Brian Hsu, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey Kwok, Nathan Smith, Michaela Schwab, Aidan Martas, Ricardo R. Munoz, Gustavo E. Medina, Ting S. Li, Paula Diaz, Daichi Hiramatsu, Brad E. Tucker, J. C. Wheeler, Xiaofeng Wang, Qian Zhai, Jujia Zhang, Anjasha Gangopadhyay, Yi Yang, Claudia P. Gutiérrez
Figure caption: Nondetection limits on the pre-explosion activity of SN 2024ggi. The typical brightness of pre-explosion outbursts of SNe IIn is indicated by the blue area (Ofek et al. 2014; Strotjohann et al. 2021). The brightness of precursor emission observed in Type II SN 2020tlf is marked with the green area (Jacobson-Galán et al. 2022), while the nondetection limit on the pre-explosion activity of Type II SN 2023ixf is represented by the green hatched area (Dong et al. 2023; Ransome et al. 2024; Rest et al. 2024).
Paper: Extended Shock Breakout and Early Circumstellar Interaction in SN 2024ggi
Authors: Manisha Shrestha, K. Azalee Bostroem, David J. Sand, Griffin Hosseinzadeh, Jennifer E. Andrews, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jeniveve Pearson, Jacob E. Jencson, M. J. Lundquist, Darshana Mehta, Aravind P. Ravi, Nicolás Meza Retamal, Stefano Valenti, Peter J. Brown, Saurabh W. Jha, Colin Macrie, Brian Hsu, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey Kwok, Nathan Smith, Michaela Schwab, Aidan Martas, Ricardo R. Munoz, Gustavo E. Medina, Ting S. Li, Paula Diaz, Daichi Hiramatsu, Brad E. Tucker, J. C. Wheeler, Xiaofeng Wang, Qian Zhai, Jujia Zhang, Anjasha Gangopadhyay, Yi Yang, Claudia P. Gutiérrez
Figure caption: Left: multiwavelength photometry of SN 2024ggi for the first 2.5 days in absolute and extinction-corrected (Milky Way + host) apparent magnitudes with no filter shifts. The dashed orange line represents the assumed explosion epoch. Right: the full multiwavelength light curve of SN 2024ggi extending to 21 days, including data from ATLAS, DLT40, Swift, Las Cumbres Observatory, and the last nondetection from GOTO (Killestein et al. 2024). The data are well sampled throughout the first 20 days including the very early rise and plateau.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Extended Shock Breakout and Early Circumstellar Interaction in SN 2024ggi
Authors: Manisha Shrestha, K. Azalee Bostroem, David J. Sand, Griffin Hosseinzadeh, Jennifer E. Andrews, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jeniveve Pearson, Jacob E. Jencson, M. J. Lundquist, Darshana Mehta, Aravind P. Ravi, Nicolás Meza Retamal, Stefano Valenti, Peter J. Brown, Saurabh W. Jha, Colin Macrie, Brian Hsu, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Lindsey Kwok, Nathan Smith, Michaela Schwab, Aidan Martas, Ricardo R. Munoz, Gustavo E. Medina, Ting S. Li, Paula Diaz, Daichi Hiramatsu, Brad E. Tucker, J. C. Wheeler, Xiaofeng Wang, Qian Zhai, Jujia Zhang, Anjasha Gangopadhyay, Yi Yang, Claudia P. Gutiérrez
Figure caption: Composite gri image of SN 2024ggi and its host galaxy NGC 3621 taken by Las Cumbres Observatory on MJD 60412.46 (+1.7 days after the explosion).
Paper: Close Encounters of Wide Binaries Induced by the Galactic Tide: Implications for Stellar Mergers and Gravitational-wave Sources
Authors: Jakob Stegmann, Alejandro Vigna-Gómez, Antti Rantala, Tom Wagg, Lorenz Zwick, Mathieu Renzo, Lieke A. C. van Son, Selma E. de Mink, Simon D. M. White
Figure caption: Schematic overview of the problem considered in this work. We study the dynamical evolution of wide binaries along their barycenter trajectory  R  =  R (t) through the Galaxy (dashed curve), denoting its projection onto the Galactic plane as  ρ  =  ρ (t). We consider one model in which the wide binaries are solely perturbed by the axisymmetric Galactic potential Φ and another one where we additionally include the impulsive effect of ambient stars impinging on the encounter sphere (solid circle) with radius R enc from the binary barycenter. The main effect of the Galactic perturbations is to torque the binary orbital angular momentum  L  leading to large-amplitude oscillations of the binary eccentricity e, and hence its peri- and apoapsis r = a(1 ∓ e), and the relative orientation ﹩\cos (i)={\hat{{\boldsymbol{e}}}}_{L}\cdot {\hat{{\boldsymbol{e}}}}_{z}﹩ of the orbital plane with respect to the Galactic frame (insets). The dimensions are not drawn to scale. The Atlas Image of the Milky Way in the near-infrared used as a background is courtesy of 2MASS/UMass/IPAC-Caltech/NASA/NSF.
Paper: Close Encounters of Wide Binaries Induced by the Galactic Tide: Implications for Stellar Mergers and Gravitational-wave Sources
Authors: Jakob Stegmann, Alejandro Vigna-Gómez, Antti Rantala, Tom Wagg, Lorenz Zwick, Mathieu Renzo, Lieke A. C. van Son, Selma E. de Mink, Simon D. M. White
Figure caption: The effect of Galactic tides in driving wide binaries to close separations. Panels (A) and (B) show the minimum separation ﹩{r}_{\min }﹩ of the binaries in our population as a function of their initial semimajor axis a 0 and the initial inclination ﹩\cos ﹩                      i 0 between their orbital plane and the Galactic plane, respectively. The minimum separation ﹩{r}_{\min }﹩ is defined as the closest distance the binary members ever achieve owing to Galactic tides over a maximum integration time of 14 Gyr, either when considering (orange circles) or when neglecting (blue plus signs) encounters with passing stars. The purple dashed line separates compact object binaries that merge owing to the emission of gravitational waves, where arrows indicate that the binaries are simulated until merging. The red shaded area shows the regime in which stellar binaries fill their Roche lobes at periapsis (P. P. Eggleton 1983); below that area they potentially collide. The black line in panel (B) forms a narrow cone defining the smallest minimum separation allowed in the torus-averaged approximation (Equation (19)) for a fiducial semimajor axis a 0 = 102 au. Black squares indicate particular example systems shown in Figures 3 and 5–7. Panel (C) shows the cumulative distribution functions (CDF), as well as the initial distribution of ﹩{r}_{\min }={a}_{0}(1-{e}_{0})﹩ following a thermal eccentricity distribution (see Section 2.4).
Paper: Close Encounters of Wide Binaries Induced by the Galactic Tide: Implications for Stellar Mergers and Gravitational-wave Sources
Authors: Jakob Stegmann, Alejandro Vigna-Gómez, Antti Rantala, Tom Wagg, Lorenz Zwick, Mathieu Renzo, Lieke A. C. van Son, Selma E. de Mink, Simon D. M. White
Figure caption: Example of a wide binary orbiting inside the Milky Way potential without stellar encounters. (A) Relative separation r of the binary members and semimajor axis a as a function of time. The gray shaded area is defined by ﹩r\lt a(1-{e}_{\max ,\sec })﹩, where ﹩{e}_{\max ,\sec }﹩ is given by Equation (19). For the secondary abscissa we calculate the secular timescale ﹩{t}_{\sec }﹩ from Equation (20). (B, C) The trajectory of the binary barycenter viewed edge-on and face-on, respectively. The black curve shows the entire trajectory over t = 14 Gyr, red highlights the last ﹩t\in [14\,{\rm{Gyr}}-{t}_{\sec },14\,{\rm{Gyr}})﹩ of it, and the star symbol indicates the final (t = 14 Gyr) position of the binary. (D) The time average 〈Φ ij 〉(t) of the tidal field components along the barycenter trajectory. Off-diagonal terms not shown here are zero or quickly decay to it. (E) The variations of the tidal field to check for the secular breakdown condition in Equation (28). The gray shaded area defines the parameter space where the condition is satisfied and large nonsecular eccentricities are possible.
Paper: Close Encounters of Wide Binaries Induced by the Galactic Tide: Implications for Stellar Mergers and Gravitational-wave Sources
Authors: Jakob Stegmann, Alejandro Vigna-Gómez, Antti Rantala, Tom Wagg, Lorenz Zwick, Mathieu Renzo, Lieke A. C. van Son, Selma E. de Mink, Simon D. M. White
Figure caption: The effect of natal kicks on the formation of wide BBHs. The dashed line shows the initial distribution of N 0 = 105 wide, massive binaries (m 1 = m 2 = 10 M ⊙) that consecutively receive two natal kicks at BH formation whose magnitudes are drawn from a Maxwellian velocity distribution with dispersion σ kick. Solid lines show the semimajor-axis distribution of all surviving BBHs, and the gray shaded area highlights the range of values simulated in this work. As a reference, we also show the orbital velocity of the BBHs (Equation (11)).
Paper: Close Encounters of Wide Binaries Induced by the Galactic Tide: Implications for Stellar Mergers and Gravitational-wave Sources
Authors: Jakob Stegmann, Alejandro Vigna-Gómez, Antti Rantala, Tom Wagg, Lorenz Zwick, Mathieu Renzo, Lieke A. C. van Son, Selma E. de Mink, Simon D. M. White
Figure caption: Five different dynamical regimes for wide binaries inside the Milky Way potential. We assume an example binary with semimajor axis a whose barycenter moves on a circular trajectory at a Galactocentric radius ρ on the Galactic plane. We set the binary masses to m 1 = m 2 = 1 M ⊙ but note that the displayed dynamical regimes are not particularly sensitive to this choice. The figure shows that our sampled range, a = 102–105 au (see Section 2.4), fully covers the spectrum where the Galactic potential can influence wide binaries on a meaningful timescale. The details of the figure are fully explained in Section 3.
Paper: Close Encounters of Wide Binaries Induced by the Galactic Tide: Implications for Stellar Mergers and Gravitational-wave Sources
Authors: Jakob Stegmann, Alejandro Vigna-Gómez, Antti Rantala, Tom Wagg, Lorenz Zwick, Mathieu Renzo, Lieke A. C. van Son, Selma E. de Mink, Simon D. M. White
Figure caption: Same as Figure 3, but for a binary undergoing a nonsecular high-eccentricity excitation after t ≈ 2.3 Gyr followed by a gravitational-wave merger. The inset to panel (A) displays the evolution of the binary eccentricity e and the dominant harmonic of the gravitational-wave frequency f GW (L. Wen 2003) through the bandwidths of LISA and LIGO/Virgo/Kagra.
Paper: Close Encounters of Wide Binaries Induced by the Galactic Tide: Implications for Stellar Mergers and Gravitational-wave Sources
Authors: Jakob Stegmann, Alejandro Vigna-Gómez, Antti Rantala, Tom Wagg, Lorenz Zwick, Mathieu Renzo, Lieke A. C. van Son, Selma E. de Mink, Simon D. M. White
Figure caption: Initial semimajor axis a 0 and minimum Galactocentric radius ﹩{\rho }_{\min }﹩ of wide binaries that get disrupted. Disruptions are defined as when the binary separation at any time in the simulation exceeds r = 10a 0 (see Section 2.1). The minimum Galactocentric radius ﹩{\rho }_{\min }﹩ is defined as the minimum of ρ of the barycenter trajectory inside the Galaxy. Gray and black shaded regions correspond to the Hill instability evaluated at that distance for binary masses m > 2 M ⊙ and m > 20 M ⊙, respectively. These limits correspond to the minimum and maximum mass in our population (see Section 2.4).
Paper: Close Encounters of Wide Binaries Induced by the Galactic Tide: Implications for Stellar Mergers and Gravitational-wave Sources
Authors: Jakob Stegmann, Alejandro Vigna-Gómez, Antti Rantala, Tom Wagg, Lorenz Zwick, Mathieu Renzo, Lieke A. C. van Son, Selma E. de Mink, Simon D. M. White
Figure caption: Same as Figure 3, but for a binary that is perturbed by stellar encounters and that gets disrupted after t ≈ 9 Gyr.
Paper: Close Encounters of Wide Binaries Induced by the Galactic Tide: Implications for Stellar Mergers and Gravitational-wave Sources
Authors: Jakob Stegmann, Alejandro Vigna-Gómez, Antti Rantala, Tom Wagg, Lorenz Zwick, Mathieu Renzo, Lieke A. C. van Son, Selma E. de Mink, Simon D. M. White
Figure caption: Same as Figure 3, but for a binary undergoing chaotic evolution.
Paper: Unveiling the Central Engine of Core-collapse Supernovae in the Local Universe: Neutron Star or Black Hole?
Authors: Maurice H. P. M. van Putten, Maryam Aghaei Abchouyeh, Massimo Della Valle
Figure caption: Venn diagram of CC-SNe (not to scale). The energetic CC-SNe Ib/c have a small fraction ﹩{\rm{\Gamma }}{\rm{^{\prime} }}﹩ producing GRB-SNe (yellow) with an additional fraction ﹩{\rm{\Gamma }}{\rm{^{\prime} }}{\rm{^{\prime} }}﹩ of failed GRB-SNe (turquoise). Both may have a dominant output in gravitational radiation (GW-SN) when powered by a rotating black hole (M. H. P. M. van Putten & A. Levinson 2003). The progenitor and remnant of the remainder (dark blue) is unknown, largely by ambiguity in their central engine (NS or BH). Similarly for the larger group of SNe II (gradient fill). The large stellar radius of their progenitors appears prohibitive for any central engine to be sufficiently long lived to successfully produce a GRB, even as some may be GW-SNe. The gradient-filled bar zooms in on SNe of Type Ic, highlighting a diversity in narrow-line (NL) and broad-line (BL) events (J. I. Maurer et al. 2010) and branching ratios Γ (Appendix A) of the latter into (L)LGRBs following A. Corsi et al. (2016, 2023).
Paper: Unveiling the Central Engine of Core-collapse Supernovae in the Local Universe: Neutron Star or Black Hole?
Authors: Maurice H. P. M. van Putten, Maryam Aghaei Abchouyeh, Massimo Della Valle
Figure caption: Distributions of CC-SNe of Types II and Ib/c by their photospheric velocity β = v ph/c and kinetic energy derived from EM observations (B. N. Ashoka et al. 1987; A. Pastorello et al. 2005; V. P. Utrobin & N. N. Chugai 2011; J. D. Lyman et al. 2016). β is derived from photospheric velocities about 1–2 months after the shock breakout time t  b . (Top panel) SNe of Type Ic stand out by their kinetic energy and photospheric velocity, especially compared to SN1987A at the far left of the distribution. (Bottom panels) Histograms of β and kinetic energy of SNe Ib/c and II indicating a clear distinction between the three in EM observations.
Paper: Unveiling the Central Engine of Core-collapse Supernovae in the Local Universe: Neutron Star or Black Hole?
Authors: Maurice H. P. M. van Putten, Maryam Aghaei Abchouyeh, Massimo Della Valle
Figure caption: (Left top panel) Radius of ISCO, R ISCO, as a function of specific angular momentum a =J/M here expressed as ﹩\hat{a}=a/M﹩—the dimensionless spin parameter of a Kerr BH. Rapidly rotating BHs have smaller R ISCO. In its lowest energy state (M. H. P. M. van Putten 2001), it facilitates strong interactions with surrounding matter via a torus magnetosphere. We use R ISCO in a radial normalization of the interaction between the BH and the surrounding high-density matter to parameterize the ensuing multimessenger radiation (5). (Right bottom panel) Spin energy E  J  as a function of ﹩\hat{a}﹩, plotted relative to the maximal spin energy of an extremal Kerr BH (﹩\hat{a}=1﹩). The threshold ﹩\hat{a}\simeq 0.44﹩ with ﹩{E}_{J}/{E}_{J}^{{\rm{\max }}}\simeq 9 \% ﹩ is the marginal suspended accretion state with no excess energy for radiation in other channels (dashed line; M. H. P. M. van Putten 2012). Higher spin parameters are required for additional radiation in GWs and MeV neutrinos. The transition to accretion from the disk is at ﹩\hat{a}\simeq 0.36﹩ (dotted line), where the rotational energy of the BH is further reduced to ﹩{E}_{J}/{E}_{J}^{{\rm{\max }}}\simeq 6 \% ﹩. Lower ﹩\hat{a}﹩ results in accretion with possible black hole spin-up. The intermediate region of ﹩0.36\lt \hat{a}\lt 0.44﹩ is a gray area in which E  J  does not allow disk accretion, but accretion from disk winds is present. (Right panel) Schematic overview of the BH spin-down/up when the BH is rotating faster/slower than the surrounding matter with no-slip boundary conditions to its torus magnetosphere and slip boundary conditions on the BH event horizon (Figure 4). The angular velocities of the BH Ω H  and surrounding matter ΩISCO at the limit of R  T  = R ISCO are shown in blue and red curves, respectively (Figure 8). The former case, Ω H  > ΩISCO, is promising for its potential to energize the surrounding matter, reprocessing this input in different radiation channels. These various radiations originate at their respective ISCO-normalized radii K (orange). The transition between the two cases is theoretically indicated by Ω H  = ΩISCO equivalent to ﹩\hat{a}\simeq 0.36﹩ (gray) and more realistically at ﹩\hat{a}\simeq 0.44﹩ (green) (M. H. P. M. van Putten 2012).
Paper: Unveiling the Central Engine of Core-collapse Supernovae in the Local Universe: Neutron Star or Black Hole?
Authors: Maurice H. P. M. van Putten, Maryam Aghaei Abchouyeh, Massimo Della Valle
Figure caption: Schematic of the ISCO-normalized BH central engine, in which radii R are normalized to R ISCO = zR  g . GW emission and magnetic winds are radiated at the effective normalized radii K GW and K  W , respectively. These are expected to satisfy the inequality K GW < K  W , provided the system is in the state of a suspended accretion sustained by a Poynting flux S emanating from the BH through Alfvén waves mediated by an inner torus magnetosphere surrounding the horizon in its lowest energy state (M. H. P. M. van Putten 2001). A relatively subdominant radiation is released in to an open outflow powering a jet. This process lasts while the BH is effectively spinning faster than the angular velocity of the ISCO. (After M. H. P. M. van Putten 1999, 2001, and M. H. P. M. van Putten & A. Levinson 2003.)